We investigate the effects of the nearby interstellar medium (ISM) on the locally measured cosmic-ray (CR) spectra. Using the G al P rop code, we explore how variations in the local gas and source distributions affect spectral features at low energies. Comparing with recent Voyager 1 measurements taken in the local ISM, we show that for a realistic interstellar gas distribution the data favor models in which there are no significant CR sources within ∼150–200 pc of the solar system, implying that the nearest dominant contributors to the low-energy CR flux are located at distances beyond this range. We find that the modeling supports the conclusion of A. C. Cummings et al. that there is a significant fraction of primary boron in its observed spectrum at low energies. Our study shows that detailed modeling of the immediate Galactic environment is required to robustly infer Galactic CR propagation parameters from local measurements and that accounting for nearby ISM structure can alleviate tensions between direct CR data and global propagation models.
",
"doi": "10.3847/1538-4357/ae4c57",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-04-10",
"series_number": "1",
"volume": "1001",
"issue": "1",
"pages": "17"
},
{
"id": "authors:ycxkr-2tn85",
"collection": "authors",
"collection_id": "ycxkr-2tn85",
"cite_using_url": "https://authors.library.caltech.edu/records/ycxkr-2tn85",
"type": "article",
"title": "Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary \u00b2H and B",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Moskalenko",
"given_name": "I. V.",
"orcid": "0000-0001-6141-458X"
},
{
"family_name": "Heikkila",
"given_name": "B. C."
},
{
"family_name": "J\u00f3hannesson",
"given_name": "G.",
"orcid": "0000-0003-1458-7036"
},
{
"family_name": "Porter",
"given_name": "T. A.",
"orcid": "0000-0002-2621-4440"
}
],
"abstract": "\n
We present the first measurements of the energy spectra of the isotopes of Galactic cosmic rays (GCRs) with nuclear charge Z = 1–14 in the very local interstellar medium (VLISM). We also update our previously published energy spectra of GCR elements in the VLISM from Z = 1–28 for a new longer time period of observations, 2013 January 1 through 2021 December 31. The observations are from the Cosmic Ray Subsystem on the Voyager 1 (V1) spacecraft and cover the Z-dependent energy range from ∼3 to 661 MeV nuc−1. The data are fit to eight models using the GCR propagation code GalProp, which differ by having four options for fragmentation and two options for production cross sections. The models are all plain diffusion models with injection spectra as power laws in rigidity, where the propagation parameters and the injection power-law index are the same for all species, and derived self-consistently and independently for each model. The VLISM energy spectra generated by the models agree reasonably well with the observed VLISM energy spectra for the elements with Z = 1–28 and with the isotopes with Z = 1–14. However, to achieve reasonable fits to the 2H and B energy spectra, it was necessary to add a primary source of 2H and B.
\n
\n
In the latter moments of 2023 July 17, the solar active region (AR) 13363, near the southwestern face of the Sun, was undergoing considerable evolution, which resulted in a significant solar energetic particle (SEP) event measured by Parker Solar Probe’s Integrated Science Investigation of the Sun (IS\u2299IS) and near-Earth spacecraft. Remote observations from GOES and CHASE captured two M5.0+ solar flares that peaked at 23:34 and 00:06 UT from the source region. In tandem, STEREO COR2 first recorded a small, narrow coronal mass ejection (CME) emerging at 22:54 UT and then saw a major halo CME emerge at 23:43 UT with a bright, rapidly expanding core and CME-driven magnetic shock with an estimated speed of ∼1400 km s−1. Parker Solar Probe was positioned at 0.65 au, near-perfectly on the nominal Parker spiral magnetic field line, which connected Earth and the AR for a 537 km s−1 ambient solar wind speed at L1. This fortuitous alignment provided the opportunity to examine how the SEP velocity dispersion, energy spectra, elemental composition, and fluence varied from 0.65 to 1 au along a shared magnetic connection to the Sun. We find a strong radial gradient, which is best characterized for H and He as r−4.0, and most surprisingly, is stronger for O and Fe, which is better described by r−5.7.
\n
\n
The 2021 October 28 solar energetic particle (SEP) event was a rare ground level enhancement (GLE) event, where secondary particles from the interactions of SEPs with the Earth's atmosphere were detected by neutron monitors on the ground. A number of papers have examined the solar signatures, neutron monitor observations, and the characteristics of the SEP protons and electrons for this event. Here we describe the heavy ion signatures, specifically O and Fe, observed by multiple spacecraft. Parker Solar Probe, Solar Terrestrial Relations Observatory-Ahead, and Advanced Composition Explorer were distributed over nearly 60° in solar longitude and 0.4 au in heliocentric distance. Despite their separations, all three spacecraft measured event-integrated O and Fe spectra, well represented by power laws, with nearly the same power-law index of approximately −1.7, which is significantly harder than most large SEP events and many GLE events. Moreover, the Fe/O abundance ratio determined from these spectra was also found to be spatially invariant over the 60° in longitude and 0.4 au in heliocentric distance. Such near uniformity is highly unusual, and only one similar occurrence was found in a previous multispacecraft. The observed Fe/O ratio of 0.39 is higher than typical for large SEP events but not unusual for GLE events.
\n
Edward Stone was a pre-eminent space scientist with an exceptional record of leading space missions and building ground-based astronomical facilities. The public face of NASA’s Voyager missions for the launch of the two probes in 1977, he served as project scientist for 50 years. Stone introduced the world to the wonders of the gas-giant planets (Jupiter, Saturn, Uranus and Neptune) in multiple press conferences, from Voyager 1’s encounter with Jupiter in 1979 to Voyager 2’s fly-by of Neptune in 1989. He also oversaw the probes entering interstellar space — the first in 2012 and the second in 2018. They continue to transmit data to Earth today.
",
"doi": "10.1038/d41586-024-02285-w",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2024-07-18",
"series_number": "8021",
"volume": "631",
"issue": "8021",
"pages": "501"
},
{
"id": "authors:e15ew-kkm87",
"collection": "authors",
"collection_id": "e15ew-kkm87",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220908-184327219",
"type": "article",
"title": "The Isotopic Abundances of Galactic Cosmic Rays with Atomic Number 29 \u2264 Z \u2264 38",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-Mark-E"
},
{
"family_name": "Rosenvinge",
"given_name": "T. T. von",
"orcid": "0000-0001-7320-4141",
"clpid": "Rosenvinge-T-T-von"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Nolfo",
"given_name": "G. A. de",
"orcid": "0000-0002-3677-074X",
"clpid": "Nolfo-G-A-de"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "The Cosmic Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer spacecraft has been operating successfully in a halo orbit about the L1 Lagrange point since late 1997. We report here the isotopic composition of the Galactic cosmic ray (GCR) elements with 29 \u2264 Z \u2264 38 derived from more than 20 years of CRIS data. Using a model of cosmic-ray transport in the Galaxy and the solar system (SS), we have derived from these observations the isotopic composition of the accelerated material at the GCR source (GCRS). Comparison of the isotopic fractions of these elements in the GCRS with corresponding fractions in the solar system gives no indication of GCRS enrichment in r-process isotopes. Since a large fraction of core-collapse supernovae (CCSNe) occur in OB associations, the fact that GCRs do not contain enhanced abundances of r-process nuclides indicates that CCSNe are not the principal source of lighter (Z \u2264 38) r-process nuclides in the solar system. This conclusion supports recent work that points to binary neutron-star mergers, rather than supernovae, as the principal source of galactic r-process isotopes.",
"doi": "10.3847/1538-4357/ac82e7",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-09-01",
"series_number": "1",
"volume": "936",
"issue": "1",
"pages": "13"
},
{
"id": "authors:rj39w-zab87",
"collection": "authors",
"collection_id": "rj39w-zab87",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210608-140607023",
"type": "article",
"title": "Magnetic field line random walk and solar energetic particle path lengths. Stochastic theory and PSP/IS\u2299IS observations",
"author": [
{
"family_name": "Chhiber",
"given_name": "R.",
"clpid": "Chhiber-R"
},
{
"family_name": "Matthaeus",
"given_name": "W. H."
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Ruffolo",
"given_name": "D."
},
{
"family_name": "Sonsrettee",
"given_name": "W."
},
{
"family_name": "Tooprakai",
"given_name": "P."
},
{
"family_name": "Seripienlert",
"given_name": "A."
},
{
"family_name": "Chuychai",
"given_name": "P."
},
{
"family_name": "Usmanov",
"given_name": "A. V."
},
{
"family_name": "Goldstein",
"given_name": "M. L."
},
{
"family_name": "McComas",
"given_name": "D. J."
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Szalay",
"given_name": "J. R."
},
{
"family_name": "Joyce",
"given_name": "C. J."
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Roelof",
"given_name": "E. C.",
"orcid": "0000-0002-2270-0652"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-Allan-W"
},
{
"family_name": "Giacalone",
"given_name": "J.",
"orcid": "0000-0002-0850-4233"
},
{
"family_name": "Schwadron",
"given_name": "N. A.",
"orcid": "0000-0002-3737-9283"
},
{
"family_name": "Mitchell",
"given_name": "D. G.",
"orcid": "0000-0003-1960-2119"
},
{
"family_name": "Hill",
"given_name": "M. E.",
"orcid": "0000-0002-5674-4936"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-Mark-E"
},
{
"family_name": "McNutt",
"given_name": "R. L.",
"orcid": "0000-0002-4722-9166"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008"
}
],
"abstract": "Context. In 2020 May-June, six solar energetic ion events were observed by the Parker Solar Probe/IS\u2299IS instrument suite at \u22480.35 AU from the Sun. From standard velocity-dispersion analysis, the apparent ion path length is \u22480.625 AU at the onset of each event. \n\nAims. We develop a formalism for estimating the path length of random-walking magnetic field lines to explain why the apparent ion path length at an event onset greatly exceeds the radial distance from the Sun for these events. \n\nMethods. We developed analytical estimates of the average increase in path length of random-walking magnetic field lines, relative to the unperturbed mean field. Monte Carlo simulations of field line and particle trajectories in a model of solar wind turbulence were used to validate the formalism and study the path lengths of particle guiding-center and full-orbital trajectories. The formalism was implemented in a global solar wind model, and the results are compared with ion path lengths inferred from IS\u2299IS observations. \n\nResults. Both a simple estimate and a rigorous theoretical formulation are obtained for field-lines' path length increase as a function of path length along the large-scale field. From simulated field line and particle trajectories, we find that particle guiding centers can have path lengths somewhat shorter than the average field line path length, while particle orbits can have substantially longer path lengths due to their gyromotion with a nonzero effective pitch angle. \n\nConclusions. The long apparent path length during these solar energetic ion events can be explained by (1) a magnetic field line path length increase due to the field line random walk and (2) particle transport about the guiding center with a nonzero effective pitch angle due to pitch angle scattering. Our formalism for computing the magnetic field line path length, accounting for turbulent fluctuations, may be useful for application to solar particle transport in general.",
"doi": "10.1051/0004-6361/202039816",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-06",
"volume": "650",
"pages": "Art. No. \tA26"
},
{
"id": "authors:p0mr3-esh29",
"collection": "authors",
"collection_id": "p0mr3-esh29",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201002-094021793",
"type": "article",
"title": "Voyager 2 Observations Near the Heliopause",
"author": [
{
"family_name": "Richardson",
"given_name": "John D.",
"orcid": "0000-0003-4041-7540",
"clpid": "Richardson-J-D"
},
{
"family_name": "Belcher",
"given_name": "John W.",
"clpid": "Belcher-J-W"
},
{
"family_name": "Burlaga",
"given_name": "Leonard F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Decker",
"given_name": "Robert B.",
"clpid": "Decker-R-B"
},
{
"family_name": "Opher",
"given_name": "Merav",
"clpid": "Opher-M"
},
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "This paper discusses plasma characteristics in the heliosheath region before the heliopause (HP), at the HP, and in the very local interstellar medium (VLISM). The Voyager 2 (V2) HP was a sharp boundary where the radial plasma currents went to background levels. The radial flow speeds derived from 53-85 keV (V1) and 28-43 keV (V2) ion data decreased about 2 years (8 AU) before the HP at V1 and V2. A speed decrease was not observed by the V2 plasma instrument until 160 days (1.5 AU) before the HP crossing when V2 entered the plasma boundary layer where the plasma density and 28-43 keV ion intensity increased. We determine the HP orientation based on the plasma flow and magnetic field data and show these observations are consistent with models predicting a blunt HP. Variations are observed in the currents observed in the VLISM; roll data from this region clearly show the plasma instrument observes the interstellar plasma and may be consistent with larger than expected VLISM temperatures near the HP.",
"doi": "10.1088/1742-6596/1620/1/012016",
"issn": "1742-6588",
"publisher": "IOP",
"publication": "Journal of Physics Conference Series",
"publication_date": "2020-09-30",
"volume": "1620",
"pages": "Art. No. 012016"
},
{
"id": "authors:sbf8x-a1b82",
"collection": "authors",
"collection_id": "sbf8x-a1b82",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200203-092721818",
"type": "article",
"title": "\u00b3He-rich Solar Energetic Particle Observations at the Parker Solar Probe and near Earth",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Bu\u010dik",
"given_name": "R.",
"orcid": "0000-0001-7381-6949"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618"
},
{
"family_name": "Ho",
"given_name": "G. C.",
"orcid": "0000-0003-1093-2066"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008"
},
{
"family_name": "Giacalone",
"given_name": "J."
},
{
"family_name": "Haggerty",
"given_name": "D. K.",
"orcid": "0000-0001-6395-8943"
},
{
"family_name": "Hill",
"given_name": "M. E.",
"orcid": "0000-0002-5674-4936"
},
{
"family_name": "Joyce",
"given_name": "C. J.",
"orcid": "0000-0002-3841-5020"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Malandraki",
"given_name": "O.",
"orcid": "0000-0002-4751-6835"
},
{
"family_name": "Matthaeus",
"given_name": "W. H.",
"orcid": "0000-0001-7224-6024"
},
{
"family_name": "McComas",
"given_name": "D. J.",
"orcid": "0000-0001-6160-1158"
},
{
"family_name": "McNutt",
"given_name": "R. L., Jr.",
"orcid": "0000-0002-4722-9166"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mitchell",
"given_name": "D. G.",
"orcid": "0000-0003-1960-2119"
},
{
"family_name": "Posner",
"given_name": "A.",
"orcid": "0000-0003-1572-8734"
},
{
"family_name": "Rankin",
"given_name": "J. S.",
"orcid": "0000-0002-8111-1444"
},
{
"family_name": "Roelof",
"given_name": "E. C.",
"orcid": "0000-0002-2270-0652"
},
{
"family_name": "Schwadron",
"given_name": "N. A.",
"orcid": "0000-0002-3737-9283"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Szalay",
"given_name": "J. R.",
"orcid": "0000-0003-2685-9801"
},
{
"family_name": "Bale",
"given_name": "S. D.",
"orcid": "0000-0002-1989-3596"
},
{
"family_name": "Case",
"given_name": "A. W.",
"orcid": "0000-0002-3520-4041"
},
{
"family_name": "Kasper",
"given_name": "J. C.",
"orcid": "0000-0002-7077-930X"
},
{
"family_name": "Korreck",
"given_name": "K. E.",
"orcid": "0000-0001-6095-2490"
},
{
"family_name": "Larson",
"given_name": "D. E.",
"orcid": "0000-0001-5030-6030"
},
{
"family_name": "MacDowall",
"given_name": "R. J.",
"orcid": "0000-0003-3112-4201"
},
{
"family_name": "Pulupa",
"given_name": "M.",
"orcid": "0000-0002-1573-7457"
},
{
"family_name": "Stevens",
"given_name": "M. L.",
"orcid": "0000-0002-7728-0085"
}
],
"abstract": "The Integrated Science Investigation of the Sun (IS\u2299IS) instrument suite on the Parker Solar Probe (PSP) spacecraft is making in situ observations of energetic ions and electrons closer to the Sun than any previous mission. Using data collected during its first two orbits, which reached perihelion distances of 0.17 au, we have searched for \u00b3He-rich solar energetic particle (SEP) events under very quiet solar minimum conditions. On 2019-110\u2013111 (April 20\u201321), \u00b3He-rich SEPs were observed at energies near 1 MeV nucleon \u207b\u00b9 in association with energetic protons, heavy ions, and electrons. This activity was also detected by the Ultra-Low-Energy Isotope Spectrometer and the Electron, Proton, and Alpha Monitor instruments on the Advanced Composition Explorer (ACE) spacecraft located near Earth, 0.99 au from the Sun. At that time, PSP and ACE were both magnetically connected to locations near the west limb of the Sun. Remote sensing measurements showed the presence of type III radio bursts and also helical jets from this region of the Sun. This combination of observations is commonly associated with \u00b3He-rich SEP acceleration on the Sun. AR 12738, which was located at Carrington coordinates from which numerous X-ray flares were observed over a period of more than 6 months, was identified as the source of the \u00b3He-rich events. This region was also the source of several other SEP events detected at PSP or ACE. Aside from the period in 2019 April, IS\u2299IS did not observe any other \u00b3He-rich SEPs during orbits 1 and 2.",
"doi": "10.3847/1538-4365/ab5963",
"issn": "1538-4365",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2020-02",
"series_number": "2",
"volume": "246",
"issue": "2",
"pages": "Art. No. 42"
},
{
"id": "authors:thaks-ave64",
"collection": "authors",
"collection_id": "thaks-ave64",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200203-092721301",
"type": "article",
"title": "Seed Population Preconditioning and Acceleration Observed by the Parker Solar Probe",
"author": [
{
"family_name": "Schwadron",
"given_name": "N. A.",
"orcid": "0000-0002-3737-9283",
"clpid": "Schwadron-N-A"
},
{
"family_name": "Bale",
"given_name": "S.",
"orcid": "0000-0002-1989-3596"
},
{
"family_name": "Bonnell",
"given_name": "J."
},
{
"family_name": "Case",
"given_name": "A.",
"orcid": "0000-0002-3520-4041"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
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{
"family_name": "Cummings",
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{
"family_name": "Davis",
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{
"family_name": "Dudok de Wit",
"given_name": "T.",
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{
"family_name": "de Wet",
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},
{
"family_name": "Desai",
"given_name": "M. I.",
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{
"family_name": "Joyce",
"given_name": "C. J.",
"orcid": "0000-0002-3841-5020"
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{
"family_name": "Goetz",
"given_name": "K."
},
{
"family_name": "Giacalone",
"given_name": "J."
},
{
"family_name": "Goerby",
"given_name": "M."
},
{
"family_name": "Harvey",
"given_name": "P."
},
{
"family_name": "Heber",
"given_name": "B.",
"orcid": "0000-0003-0960-5658"
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{
"family_name": "Hill",
"given_name": "M. E.",
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{
"family_name": "Karavolos",
"given_name": "M."
},
{
"family_name": "Kasper",
"given_name": "J. C.",
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{
"family_name": "Korreck",
"given_name": "K.",
"orcid": "0000-0001-6095-2490"
},
{
"family_name": "Larson",
"given_name": "D."
},
{
"family_name": "Livi",
"given_name": "R."
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Malandraki",
"given_name": "O."
},
{
"family_name": "MacDowall",
"given_name": "R.",
"orcid": "0000-0003-3112-4201"
},
{
"family_name": "Malaspina",
"given_name": "D.",
"orcid": "0000-0003-1191-1558"
},
{
"family_name": "Matthaeus",
"given_name": "W. H.",
"orcid": "0000-0001-7224-6024"
},
{
"family_name": "McComas",
"given_name": "D. J.",
"orcid": "0000-0001-6160-1158"
},
{
"family_name": "McNutt",
"given_name": "R. L., Jr."
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
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{
"family_name": "Mitchell",
"given_name": "D. G.",
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},
{
"family_name": "Mays",
"given_name": "L."
},
{
"family_name": "Niehof",
"given_name": "J. T."
},
{
"family_name": "Odstrcil",
"given_name": "D."
},
{
"family_name": "Pulupa",
"given_name": "M.",
"orcid": "0000-0002-1573-7457"
},
{
"family_name": "Poduval",
"given_name": "B."
},
{
"family_name": "Rankin",
"given_name": "J. S.",
"orcid": "0000-0002-8111-1444"
},
{
"family_name": "Roelof",
"given_name": "E. C."
},
{
"family_name": "Stevens",
"given_name": "M.",
"orcid": "0000-0002-7728-0085"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Szalay",
"given_name": "J. R.",
"orcid": "0000-0003-2685-9801"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
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{
"family_name": "Winslow",
"given_name": "R."
},
{
"family_name": "Whittlesey",
"given_name": "P."
}
],
"abstract": "A series of solar energetic particle (SEP) events was observed by the Integrated Science Investigation of the Sun (IS\u2299IS) on the Parker Solar Probe (PSP) during the period from 2019 April 18 through 24. The PSP spacecraft was located near 0.48 au from the Sun on Parker spiral field lines that projected out to 1 au within ~25\u00b0 of the near-Earth spacecraft. These SEP events, though small compared to historically large SEP events, were among the largest observed thus far in the PSP mission and provide critical information about the space environment inside 1 au during SEP events. During this period, the Sun released multiple coronal mass ejections (CMEs). One of these CMEs observed was initiated on 2019 April 20 at 01:25 UTC, and the interplanetary CME (ICME) propagated out and passed over the PSP spacecraft. Observations by the Electromagnetic Fields Investigation show that the magnetic field structure was mostly radial throughout the passage of the compression region and the plasma that followed, indicating that PSP did not directly observe a flux rope internal to the ICME, consistent with the location of PSP on the ICME flank. Analysis using relativistic electrons observed near Earth by the Electron, Proton and Alpha Monitor on the Advanced Composition Explorer demonstrates the presence of electron seed populations (40\u2013300 keV) during the events observed. The energy spectrum of the IS\u2299IS-observed proton seed population below 1 MeV is close to the limit of possible stationary-state plasma distributions out of equilibrium. IS\u2299IS observations reveal the enhancement of seed populations during the passage of the ICME, which likely indicates a key part of the preacceleration process that occurs close to the Sun.",
"doi": "10.3847/1538-4365/ab5527",
"issn": "1538-4365",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2020-02",
"series_number": "2",
"volume": "246",
"issue": "2",
"pages": "Art. No. 33"
},
{
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"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200203-131825142",
"type": "article",
"title": "Observations of the 2019 April 4 Solar Energetic Particle Event at the Parker Solar Probe",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
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{
"family_name": "Christian",
"given_name": "E. R.",
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{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
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{
"family_name": "Cummings",
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"clpid": "Cummings-A-C"
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{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008"
},
{
"family_name": "Giacalone",
"given_name": "J."
},
{
"family_name": "Hill",
"given_name": "M. E.",
"orcid": "0000-0002-5674-4936"
},
{
"family_name": "Joyce",
"given_name": "C. J.",
"orcid": "0000-0002-3841-5020"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
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{
"family_name": "Malandraki",
"given_name": "O.",
"orcid": "0000-0002-4751-6835"
},
{
"family_name": "Matthaeus",
"given_name": "W. H.",
"orcid": "0000-0001-7224-6024"
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{
"family_name": "McComas",
"given_name": "D. J.",
"orcid": "0000-0001-6160-1158"
},
{
"family_name": "McNutt",
"given_name": "R. L., Jr."
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
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{
"family_name": "Mitchell",
"given_name": "D. G.",
"orcid": "0000-0003-1960-2119"
},
{
"family_name": "Posner",
"given_name": "A.",
"orcid": "0000-0003-1572-8734"
},
{
"family_name": "Rankin",
"given_name": "J. S.",
"orcid": "0000-0002-8111-1444"
},
{
"family_name": "Roelof",
"given_name": "E. C."
},
{
"family_name": "Schwadron",
"given_name": "N. A.",
"orcid": "0000-0002-3737-9283"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
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{
"family_name": "Szalay",
"given_name": "J. R.",
"orcid": "0000-0003-2685-9801"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128"
},
{
"family_name": "Vourlidas",
"given_name": "A.",
"orcid": "0000-0002-8164-5948"
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{
"family_name": "Bale",
"given_name": "S. D.",
"orcid": "0000-0002-1989-3596"
},
{
"family_name": "MacDowall",
"given_name": "R. J.",
"orcid": "0000-0003-3112-4201"
},
{
"family_name": "Pulupa",
"given_name": "M.",
"orcid": "0000-0002-1573-7457"
},
{
"family_name": "Kasper",
"given_name": "J. C.",
"orcid": "0000-0002-7077-930X"
},
{
"family_name": "Allen",
"given_name": "R. C.",
"orcid": "0000-0003-2079-5683"
},
{
"family_name": "Case",
"given_name": "A. W.",
"orcid": "0000-0002-3520-4041"
},
{
"family_name": "Korreck",
"given_name": "K. E.",
"orcid": "0000-0001-6095-2490"
},
{
"family_name": "Livi",
"given_name": "R.",
"orcid": "0000-0002-0396-0547"
},
{
"family_name": "Stevens",
"given_name": "M. L.",
"orcid": "0000-0002-7728-0085"
},
{
"family_name": "Whittlesey",
"given_name": "P.",
"orcid": "0000-0002-7287-5098"
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{
"family_name": "Poduval",
"given_name": "B.",
"orcid": "0000-0003-1258-0308"
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],
"abstract": "A solar energetic particle event was detected by the Integrated Science Investigation of the Sun (IS\u2299IS) instrument suite on Parker Solar Probe (PSP) on 2019 April 4 when the spacecraft was inside of 0.17 au and less than 1 day before its second perihelion, providing an opportunity to study solar particle acceleration and transport unprecedentedly close to the source. The event was very small, with peak 1 MeV proton intensities of ~0.3 particles (cm\u00b2 sr s MeV)\u207b\u00b9, and was undetectable above background levels at energies above 10 MeV or in particle detectors at 1 au. It was strongly anisotropic, with intensities flowing outward from the Sun up to 30 times greater than those flowing inward persisting throughout the event. Temporal association between particle increases and small brightness surges in the extreme-ultraviolet observed by the Solar TErrestrial RElations Observatory, which were also accompanied by type III radio emission seen by the Electromagnetic Fields Investigation on PSP, indicates that the source of this event was an active region nearly 80\u00b0 east of the nominal PSP magnetic footpoint. This suggests that the field lines expanded over a wide longitudinal range between the active region in the photosphere and the corona.",
"doi": "10.3847/1538-4365/ab5712",
"issn": "1538-4365",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2020-02",
"series_number": "2",
"volume": "246",
"issue": "2",
"pages": "Art. No. 35"
},
{
"id": "authors:87qdd-8eb27",
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"collection_id": "87qdd-8eb27",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200203-104219201",
"type": "article",
"title": "Energetic Particle Increases Associated with Stream Interaction Regions",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
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{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937"
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{
"family_name": "Cummings",
"given_name": "A. C.",
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{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008"
},
{
"family_name": "Giacalone",
"given_name": "J."
},
{
"family_name": "Hill",
"given_name": "M. E.",
"orcid": "0000-0002-5674-4936"
},
{
"family_name": "Joyce",
"given_name": "C. J.",
"orcid": "0000-0002-3841-5020"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Matthaeus",
"given_name": "W. H.",
"orcid": "0000-0001-7224-6024"
},
{
"family_name": "McComas",
"given_name": "D. J.",
"orcid": "0000-0001-6160-1158"
},
{
"family_name": "McNutt",
"given_name": "R. L., Jr."
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mitchell",
"given_name": "D. G.",
"orcid": "0000-0003-1960-2119"
},
{
"family_name": "Rankin",
"given_name": "J. S.",
"orcid": "0000-0002-8111-1444"
},
{
"family_name": "Roelof",
"given_name": "E. C."
},
{
"family_name": "Schwadron",
"given_name": "N. A.",
"orcid": "0000-0002-3737-9283"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Szalay",
"given_name": "J. R.",
"orcid": "0000-0003-2685-9801"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128"
},
{
"family_name": "Allen",
"given_name": "R. C.",
"orcid": "0000-0003-2079-5683"
},
{
"family_name": "Ho",
"given_name": "G. C."
},
{
"family_name": "Jian",
"given_name": "L. K.",
"orcid": "0000-0002-6849-5527"
},
{
"family_name": "Lario",
"given_name": "D.",
"orcid": "0000-0002-3176-8704"
},
{
"family_name": "Odstrcil",
"given_name": "D."
},
{
"family_name": "Bale",
"given_name": "S. D.",
"orcid": "0000-0002-1989-3596"
},
{
"family_name": "Badman",
"given_name": "S. T.",
"orcid": "0000-0002-6145-436X"
},
{
"family_name": "Pulupa",
"given_name": "M.",
"orcid": "0000-0002-1573-7457"
},
{
"family_name": "MacDowall",
"given_name": "R. J.",
"orcid": "0000-0003-3112-4201"
},
{
"family_name": "Kasper",
"given_name": "J. C.",
"orcid": "0000-0002-7077-930X"
},
{
"family_name": "Case",
"given_name": "A. W.",
"orcid": "0000-0002-3520-4041"
},
{
"family_name": "Korreck",
"given_name": "K. E.",
"orcid": "0000-0001-6095-2490"
},
{
"family_name": "Larson",
"given_name": "D. E."
},
{
"family_name": "Livi",
"given_name": "Roberto"
},
{
"family_name": "Stevens",
"given_name": "M. L.",
"orcid": "0000-0002-7728-0085"
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{
"family_name": "Whittlesey",
"given_name": "Phyllis"
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],
"abstract": "The Parker Solar Probe was launched on 2018 August 12 and completed its second orbit on 2019 June 19 with perihelion of 35.7 solar radii. During this time, the Energetic Particle Instrument-Hi (EPI-Hi, one of the two energetic particle instruments comprising the Integrated Science Investigation of the Sun, IS\u2299IS) measured seven proton intensity increases associated with stream interaction regions (SIRs), two of which appear to be occurring in the same region corotating with the Sun. The events are relatively weak, with observed proton spectra extending to only a few MeV and lasting for a few days. The proton spectra are best characterized by power laws with indices ranging from \u22124.3 to \u22126.5, generally softer than events associated with SIRs observed at 1 au and beyond. Helium spectra were also obtained with similar indices, allowing He/H abundance ratios to be calculated for each event. We find values of 0.016\u20130.031, which are consistent with ratios obtained previously for corotating interaction region events with fast solar wind \u2264 600 km s\u207b\u00b9. Using the observed solar wind data combined with solar wind simulations, we study the solar wind structures associated with these events and identify additional spacecraft near 1 au appropriately positioned to observe the same structures after some corotation. Examination of the energetic particle observations from these spacecraft yields two events that may correspond to the energetic particle increases seen by EPI-Hi earlier.",
"doi": "10.3847/1538-4365/ab4c38",
"issn": "1538-4365",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2020-02",
"series_number": "2",
"volume": "246",
"issue": "2",
"pages": "Art. No. 20"
},
{
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"collection_id": "1bfnf-pry08",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200203-092721619",
"type": "article",
"title": "Energetic Particle Observations from the Parker Solar Probe Using Combined Energy Spectra from the IS\u2299IS Instrument Suite",
"author": [
{
"family_name": "Joyce",
"given_name": "C. J.",
"orcid": "0000-0002-3841-5020",
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{
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"given_name": "D. J.",
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{
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"given_name": "E. R.",
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"clpid": "Christian-E-R"
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{
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"given_name": "N. A.",
"orcid": "0000-0002-3737-9283",
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{
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{
"family_name": "McNutt",
"given_name": "R. L., Jr.",
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{
"family_name": "Cohen",
"given_name": "C. M. S.",
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{
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"given_name": "R. A.",
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{
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{
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{
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{
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{
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{
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{
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{
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"given_name": "J. S.",
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{
"family_name": "Desai",
"given_name": "M. I.",
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"clpid": "Desai-M-I"
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{
"family_name": "Giacalone",
"given_name": "J.",
"clpid": "Giacalone-J"
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{
"family_name": "Matthaeus",
"given_name": "W. H.",
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}
],
"abstract": "The Integrated Science Investigations of the Sun (IS\u2299IS) instrument suite includes two Energetic Particle instruments: EPI-Hi, designed to measure ions from ~1 to 200 MeV nuc\u207b\u00b9, and EPI-Lo, designed to measure ions from ~20 to ~15 MeV nuc\u207b\u00b9. We present an analysis of eight energetic proton events observed across the energy range of both instruments during Parker Solar Probe's (PSP) first two orbits in order to examine their combined energy spectra. Background corrections are applied to help resolve spectral breaks between the two instruments and are shown to be effective. In doing so we demonstrate that even in the early stages of calibration, IS\u2299IS is capable of producing reliable spectral observations across broad energy ranges. In addition to making groundbreaking measurements very near the Sun, IS\u2299IS also characterizes energetic particle populations over a range of heliocentric distances inside 1 au. During the first two orbits, IS\u2299IS observed energetic particle events from a single corotating interaction region (CIR) at three different distances from the Sun. The events are separated by two Carrington rotations and just 0.11 au in distance; however, the relationship shown between proton intensities and proximity of the spacecraft to the source region shows evidence of the importance of transport effects on observations of energetic particles from CIRs. Future IS\u2299IS observations of similar events over larger distances will help disentangle the effects of CIR-related acceleration and transport. We apply similar spectral analyses to the remaining five events, including four that are likely related to stream interaction regions (SIRs) and one solar energetic particle (SEP) event.",
"doi": "10.3847/1538-4365/ab5948",
"issn": "1538-4365",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2020-02",
"series_number": "2",
"volume": "246",
"issue": "2",
"pages": "Art. No. 41"
},
{
"id": "authors:s0bt8-xes74",
"collection": "authors",
"collection_id": "s0bt8-xes74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191202-155700225",
"type": "article",
"title": "ACR Proton Acceleration Associated with Reconnection Processes beyond the Heliospheric Termination Shock",
"author": [
{
"family_name": "Zhao",
"given_name": "L.-L.",
"orcid": "0000-0002-4299-0490",
"clpid": "Zhao-Lingling"
},
{
"family_name": "Zank",
"given_name": "G. P.",
"orcid": "0000-0002-4642-6192",
"clpid": "Zank-G-P"
},
{
"family_name": "Hu",
"given_name": "Q.",
"orcid": "0000-0002-7570-2301",
"clpid": "Hu-Qiang"
},
{
"family_name": "Chen",
"given_name": "Y.",
"orcid": "0000-0002-0065-7622",
"clpid": "Chen-Yu"
},
{
"family_name": "Adhikari",
"given_name": "L.",
"orcid": "0000-0003-1549-5256",
"clpid": "Adhikari-L"
},
{
"family_name": "leRoux",
"given_name": "J. A.",
"orcid": "0000-0001-9199-2890",
"clpid": "leRoux-J-A"
},
{
"family_name": "Cummings",
"given_name": "A.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
}
],
"abstract": "One of the curious observations from the Voyagers is that the intensity of anomalous cosmic rays (ACRs) did not peak at the heliospheric termination shock (HTS) but instead a short distance (within ~1 au) downstream of the HTS. One possible explanation is that the interaction of the wavy heliospheric current sheet with the HTS enhances magnetic reconnection and generates numerous small-scale magnetic flux ropes in the heliosheath immediately downstream of the HTS. Charged particles are accelerated in this region due to Fermi acceleration and the reconnection electric field. In this work, we provide observational evidence of the presence of magnetic flux ropes in the heliosheath region just downstream of the HTS using a wavelet analysis of the reduced magnetic helicity and Grad\u2013Shafranov reconstruction techniques. The Zank et al. kinetic transport theory for particles propagating through the magnetic islands region is employed to fit the observed energetic proton intensities in the post-HTS region. Our modeling results agree reasonably well with the observations, which suggests that stochastic acceleration via reconnection processes can explain the ACR proton peak beyond the HTS.",
"doi": "10.3847/1538-4357/ab4db4",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-12-01",
"series_number": "2",
"volume": "886",
"issue": "2",
"pages": "Art. No. 144"
},
{
"id": "authors:85fpw-hjk26",
"collection": "authors",
"collection_id": "85fpw-hjk26",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190926-164717298",
"type": "article",
"title": "Cosmic ray measurements from Voyager 2 as it crossed into interstellar space",
"author": [
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "Bryant C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "Nand",
"clpid": "Lal-Nand"
}
],
"abstract": "The interaction of the interstellar and solar winds is complex, as revealed by differences in intensities and anisotropies of low-energy ions (>0.5\u2009MeV per nucleon) originating inside the heliosphere and those of higher-energy Galactic cosmic rays (>70\u2009MeV per nucleon) originating outside, in the Milky Way. On 5 November 2018, Voyager 2 observed a sharp decrease in the intensity of low-energy ions and a simultaneous increase in the intensity of cosmic rays, indicating that Voyager 2 had crossed the heliopause at 119\u2009au and entered interstellar space about six years after Voyager 1. Unlike Voyager 1, which found that two interstellar flux tubes had invaded the heliosheath and served as precursors to the heliopause, Voyager 2 found no similar precursors. However, just beyond the heliopause Voyager 2 discovered a boundary layer, in which low-energy particles streamed outward along the magnetic field and cosmic ray intensities were only 90% of those further out.",
"doi": "10.1038/s41550-019-0928-3",
"issn": "2397-3366",
"publisher": "Nature Publishing Group",
"publication": "Nature Astronomy",
"publication_date": "2019-11",
"series_number": "11",
"volume": "3",
"issue": "11",
"pages": "1013-1018"
},
{
"id": "authors:y2zab-jyc23",
"collection": "authors",
"collection_id": "y2zab-jyc23",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190729-091757335",
"type": "book_section",
"title": "Elemental Source Composition Measurements and the Origin of Galactic Cosmic Rays",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "We present measurements of the elemental abundances of ultra-heavy (Z>29) cosmic rays made by the CRIS instrument on NASA's ACE satellite. The data set corresponds to 7406 days of data collection from December 4, 1997 through Feb. 18, 2019. We detected a total of 1205 ultra-heavy nuclei in the charge range of Z=30-40. The charge resolution that we obtain shows essentially complete separation of the elements over this charge range. We derive preliminary source abundances from these measurements. These source abundances show that the ordering of refractory and volatile elements with atomic mass is greatly improved when compared to a mix of massive star outflow plus SN ejecta with normal ISM, rather than with only normal ISM. Additionally, in this ordering the refractory and volatile elements have similar slopes and refractory elements are preferentially accelerated by a factor of ~4. The measured abundances support a model in which cosmic ray source material is a mix of massive star outflow plus supernova ejecta and normal ISM, consistent with conclusions reached from the SuperTIGER high-altitude balloon measurements.",
"publisher": "SISSA",
"publication_date": "2019-07"
},
{
"id": "authors:eg4ca-pqa21",
"collection": "authors",
"collection_id": "eg4ca-pqa21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190821-080755739",
"type": "book_section",
"title": "Voyager 2 Observations of the Anisotropy of Anomalous Cosmic Rays in the Heliosheath",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lai",
"given_name": "N.",
"clpid": "Lai-N"
},
{
"family_name": "Richardson",
"given_name": "J. D.",
"orcid": "0000-0003-4041-7540",
"clpid": "Richardson-J-D"
}
],
"abstract": "We have analyzed data collected from the Cosmic Ray Subsystem (CRS) instrument (Stone et al., 1977) on the Voyager 2 (V2) spacecraft during calibration manuevers for the magnetic field instrument while the spacecraft was located in the inner heliosheath of the heliosphere. We find that there is a diffusive anisotropy in the intensity of \u223c0.5-35 MeV particles (mostly protons) that indicates that there exists a diffusive flow of these particles from the flank or tail of the heliosphere towards the nose and is slightly equatorward as well. This work supports the conclusion of an earlier, similar, but more restricted study (Stone et al., 2017) that the acceleration site of anomalous cosmic rays is back along the flank or tail of the solar wind termination shock.",
"publisher": "SISSA",
"publication_date": "2019-07"
},
{
"id": "authors:cx7sq-wc626",
"collection": "authors",
"collection_id": "cx7sq-wc626",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190821-075835551",
"type": "book_section",
"title": "27-Day Modulation of Cosmic Ray Intensities During the Last Two Solar Minima",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "Variations in both anomalous cosmic ray (ACR) and galactic cosmic ray (GCR) intensities at the solar rotation period (\u223c27 days) are often observed, and appear throughout much of 2016 into 2019 during the present A>0 polarity solar minimum. During the previous A<0 solar minimum, such variations were evident at energies from a few MeV to many GeV from mid-2007 through late 2008, and were much larger for ACRs than for GCRs at comparable energy. The particle intensities had an inverse power-law correlation with the solar wind speed, intensity peaks occurred only near alternate crossings of the heliospheric current sheet, and the variations in amplitudes were larger than typical for an A<0 epoch. The heliospheric environment was unusual compared with earlier cycles, with lower solar wind dynamic pressure, weaker interplanetary magnetic field strength, and record-setting GCR intensities. The present high-energy GCR intensities are higher than ever before reported in an A>0 cycle (although lower than in several A<0 cycles), indicating that unusual modulation conditions still prevail. \nUsing high statistical precision measurements from the ACE spacecraft along with neutron monitor data, we present observations of the 27-day intensity variations in both ACRs and GCRs during the last two solar minima and describe how they depend on particle energy, rigidity, and spectrum, and on interplanetary conditions such as solar wind speed, magnetic field strength, andmcurrent sheet tilt. We compare the variations observed in this cycle with those in the previous opposite polarity cycle and discuss implications for particle transport in the heliosphere.",
"publisher": "SISSA",
"publication_date": "2019-07"
},
{
"id": "authors:4bqp6-1fh76",
"collection": "authors",
"collection_id": "4bqp6-1fh76",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190321-114830889",
"type": "article",
"title": "Galactic Cosmic-Ray Anisotropies: Voyager 1 in the Local Interstellar Medium",
"author": [
{
"family_name": "Rankin",
"given_name": "J. S.",
"orcid": "0000-0002-8111-1444",
"clpid": "Rankin-J-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McComas",
"given_name": "D. J.",
"orcid": "0000-0001-6160-1158",
"clpid": "McComas-D-J"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-Nand"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
}
],
"abstract": "Since crossing the heliopause on 2012 August 25, Voyager 1 observed reductions in galactic cosmic ray count rates caused by a time-varying depletion of particles with pitch angles near 90\u00b0, while intensities of particles with other pitch angles remain unchanged. Between late 2012 and mid-2017, three large-scale events occurred, lasting from ~100 to ~630 days. Omnidirectional and directional high-energy data from Voyager 1's Cosmic Ray Subsystem are used to report cosmic ray intensity variations. Omnidirectional (\u227320 MeV) proton-dominated measurements show up to a 3.8% intensity reduction. Bidirectional (\u227370 MeV) proton-dominated measurements taken from various spacecraft orientations provide insight about the depletion region's spatial properties. We characterize the anisotropy as a \"notch\" in an otherwise uniform pitch angle distribution of varying depth and width centered about 90\u00b0 in pitch angle space. The notch averages 22\u00b0 wide and 15% deep, signifying a depletion region that is broad and shallow. There are indications that the anisotropy is formed by a combination of magnetic trapping and cooling downstream of solar-induced transient disturbances in a region that is also likely influenced by the highly compressed fields near the heliopause.",
"doi": "10.3847/1538-4357/ab041f",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-03-01",
"series_number": "1",
"volume": "873",
"issue": "1",
"pages": "Art. No. 46"
},
{
"id": "authors:5x61c-yn009",
"collection": "authors",
"collection_id": "5x61c-yn009",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181025-112020309",
"type": "article",
"title": "Voyager 2 Observations of Plasma and Pressure Pulses",
"author": [
{
"family_name": "Richardson",
"given_name": "John D.",
"orcid": "0000-0003-4041-7540",
"clpid": "Richardson-J-D"
},
{
"family_name": "Belcher",
"given_name": "John W.",
"clpid": "Belcher-J-W"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Decker",
"given_name": "Robert",
"clpid": "Decker-R"
},
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "This paper provides the latest data from Voyager 2 on plasma characteristics in the heliosheath including the observations of pressure waves in the plasma and particle data. Models and observations show that solar transients drive pressure waves through the heliosphere. Pressure pulses that could drive heliosheath waves are observed near the previous solar maximum upstream of the termination shock. We show that the most recent data is consistent with the presence of pressure waves and compare the heliosheath waves with the pressure increases in the heliosheath. The magnetic field is better correlated with density and galactic cosmic ray intensities in the supersonic solar wind than in the heliosheath. The galactic cosmic rays are correlated with the plasma and particles with a ~30-day lag in both the supersonic wind and heliosheath.",
"doi": "10.1088/1742-6596/1100/1/012019",
"issn": "1742-6596",
"publisher": "IOP",
"publication": "Journal of Physics: Conference Series",
"publication_date": "2018-10-24",
"volume": "1100",
"pages": "Art. No. 012019"
},
{
"id": "authors:ahn06-d5974",
"collection": "authors",
"collection_id": "ahn06-d5974",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180921-095050945",
"type": "article",
"title": "Elemental Composition at the Cosmic-Ray Source Derived from the ACE-CRIS Instrument. I. _6C to _(28)Ni",
"author": [
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "We report new elemental source abundances from _6C to _(28)Ni for galactic cosmic rays, using observations from the Cosmic Ray Isotope Spectrometer (CRIS) on board the NASA Advanced Composition Explorer spacecraft. Abundances were calculated using CRIS energy spectra at energies below 550 MeV/nucleon from the 1997\u201398 and 2009\u201310 solar-minimum periods, as well as from the 2001\u201303 solar-maximum period. These new results, when combined with results for heavier elements reported in a forthcoming paper, are consistent with a model of galactic cosmic-ray origin where nuclei found in interstellar grains are accelerated preferentially over those found in interstellar gas, with this acceleration happening in OB associations.",
"doi": "10.3847/1538-4357/aad867",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2018-09-20",
"series_number": "1",
"volume": "865",
"issue": "1",
"pages": "Art. No. 69"
},
{
"id": "authors:5me0w-mkc17",
"collection": "authors",
"collection_id": "5me0w-mkc17",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-081707376",
"type": "monograph",
"title": "Voyager 1 Measurements Beyond the Heliopause of Galactic Cosmic Ray Helium, Boron, Carbon, Oxygen, Magnesium, Silicon and Iron Nuclei with Energies 0.5 to >1.5 GeV/nuc",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-Nand"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
}
],
"abstract": "We have obtained the energy spectra of cosmic ray He, B, C, O, Mg, S and Fe nuclei in the range 0.5-1.5 GeV/nuc and above using the penetrating particle mode of the High Energy Telescope, part of the Cosmic Ray Science (CRS) experiment on Voyagers 1 and 2. The data analysis procedures are the same as those used to obtain similar spectra from the identical V2 HET telescope while it was in the heliosphere between about 23 and 54 AU. The time period of analysis includes 4 years of data beyond the heliopause (HP). These new interstellar spectra are compared with various earlier experiments at the same energies at the Earth to determine the solar modulation parameter, \u03a6. These new spectra are also compared with recent measurements of the spectra of the same nuclei measured by the same telescope at low energies. It is found that the ratio of intensities at 100 MeV/nuc to those at 1.0 GeV/nuc are significantly Z dependent. Some of this Z dependence can be explained by the Z\u00b2 dependence of energy loss by ionization in the 7-10 g/cm\u00b2 of interstellar H and He traversed by cosmic rays of these energies in the galaxy; some by the Z dependent loss due to nuclear interactions in this same material; some by possible differences in the source spectra of these nuclei and some by the non-uniformity of the source distribution and propagation conditions. The observed features of the spectra, also including a Z dependence of the peak intensities of the various nuclei, pose interesting problems related to the propagation and source distribution of these cosmic rays.",
"doi": "10.48550/arXiv.1712.02818",
"publisher": "arXiv",
"publication_date": "2017-12-07"
},
{
"id": "authors:gasw7-5j711",
"collection": "authors",
"collection_id": "gasw7-5j711",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122924831",
"type": "book_section",
"title": "Anisotropy of Anomalous Cosmic Rays Observed by Voyager 2 in the Heliosheath",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-Nand"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "Voyager 2 (V2) has been observing anomalous cosmic rays (ACRs) in the heliosheath since August 2007 when V2 crossed the termination shock of the supersonic solar wind. We use the counting rate of ~0.5-35 MeV protons collected during periods when the spacecraft was rolling about the axis pointed to the Earth to infer their direction of flow. The observed flow velocity is the combination of the flow due to motion of heliosheath plasma and a diffusive flow due to a gradient in the ACR intensity. The latitudinal component of the flow (N component) agrees with the convective flow due to the heliospheric plasma flow as determined by the plasma instrument on V2. However, the tangential component of the flow (T component) is smaller than the predicted convective flow, consistent with an intensity gradient in the +T direction and a diffusive flow of ACRs from a source located in the +T direction. This would be consistent with models predicting that the acceleration of higher energy ACRs occurs along the flanks or tail of the heliosphere. A similar result was obtained by analysis of the V1 magrol data during V1's journey through the heliosheath [1].",
"doi": "10.22323/1.301.0057",
"publisher": "SISSA",
"publication_date": "2017-07"
},
{
"id": "authors:jn2h5-yxv79",
"collection": "authors",
"collection_id": "jn2h5-yxv79",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122925836",
"type": "book_section",
"title": "Reanalyzing Inferred High Energy Ionic Charge States for Solar Energetic Particle Events from 2005-2016 with ACE and STEREO",
"author": [
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Sollitt",
"given_name": "L. S.",
"clpid": "Sollitt-L-S"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "We have estimated mean high-energy ionic charge states of solar energetic particles (SEPs) using the Sollitt et al. (2008) method. In our analysis, the method applies to abundant elements (e.g. N, O, Ne, Mg, Si, and Fe) in SEP events at the energy ranges covered by the STEREO/LET instrument (e.g. 2.7-70 MeV/nuc for Fe) and the ACE/SIS instrument (e.g. 11-168 MeV/nuc for Fe). The method starts by fitting SEP time-intensity profiles during the decay phase of a given, large SEP event in order to obtain energy-dependent decay times. The energy dependence of intensity decay times for a given element in an SEP event is combined with its assumed average atomic mass and an assumed average charge state of 5.9 for carbon as a reference element. The mean charge state for each element is then estimated from the relationship between the energy dependence of its decay times to that for carbon and all other elements in the event. The method has yielded charge states for 8 SEP events using ACE data, 5 SEP events with STEREO A data, and 4 SEP events with STEREO B data through 2015. Calculations for events before 2005 by Sollitt et al. using ACE data also incorporated helium time intensity profile fits, with an assumed charge state of 2, but later calculations dropped helium as a reference element for simplicity, as the calculations were first generalized to later events and to STEREO data. In this paper, we restore helium in order to refine the calculations and compare with the earlier results. In particular, we will focus on the 8 March 2012 event with ACE/SIS data and the 28 September 2012 event with STEREO/LET data. Additionally, other charge state measurements using a geomagnetic rigidity cutoff technique yielded correlations between charge states and Fe/O ratio as well as to observed source solar longitudes. We will use the inferred charge state reanalysis to investigate whether these correlations are also present in ACE and STEREO data.",
"doi": "10.22323/1.301.0097",
"publisher": "SISSA",
"publication_date": "2017-07"
},
{
"id": "authors:7bw79-21415",
"collection": "authors",
"collection_id": "7bw79-21415",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122926202",
"type": "book_section",
"title": "Magnetic Fluctuations and Peculiar Anisotropy Oscillations in the 23 July 2012 SEP Event",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The pitch-angle distributions of solar energetic particles (SEPs) provide a wealth of information about particle transport through interplanetary space, and depend on the magnetic field strength, topology, and turbulence at remote heliospheric locations. The Low Energy Telescope (LET) on STEREO measures angular distributions in the ecliptic for SEP ions from protons to iron with energies of about 2--12 MeV/nucleon. At the onset of the 23 July 2012 extreme SEP event, a beamed distribution was observed at STEREO-Ahead using LET. We have previously reported apparent \"oscillations\" in the pitch-angle width of this beam when using simultaneous particle and magnetic field measurements at a 1-minute cadence. We have now determined that this behavior is largely a result of the effects of magnetic turbulence on the calculated particle pitch angle distributions. The locally measured magnetic field direction varies relatively rapidly, while the energetic particle distribution is governed by magnetic fields averaged over much larger spatial and temporal scales than represented by solar wind measurements at the same cadence. Similar behavior in earlier events has been reported by others and analyzed in the framework of quasilinear theory.",
"doi": "10.22323/1.301.0144",
"publisher": "SISSA",
"publication_date": "2017-07"
},
{
"id": "authors:mz711-4fe02",
"collection": "authors",
"collection_id": "mz711-4fe02",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122926410",
"type": "book_section",
"title": "Recent Results from the Cosmic Ray Isotope Spectrometer on NASA's Advanced Composition Explorer",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The Advanced Composition Explorer (ACE), which carries instrumentation for making high-precision measurements of the charge and mass of energetic nuclei between \u223c1 keV/nuc and \u223c1 GeV/nuc, was launched in August 1997 into an orbit about the L1 Lagrangian point 1.5 million km sunward of the Earth. From this vantage point, ACE collects data that are used for a wide range of studies in galactic and heliospheric physics. The ACE spacecraft and instruments are, for the most part, continuing to perform very well and to extend their data sets. The long mission duration, which is already almost an order of magnitude greater than the two years that was nominally required of ACE, has made it possible to address science topics beyond those envisioned when the mission was proposed. In this paper we address several topics to which ACE's Cosmic Ray Isotope Spectrometer (CRIS) is contributing in the area of galactic cosmic radiation. CRIS has been able to make measurements of extremely rare species, including the primary radioactive nuclide 60Fe and a number of stable \"ultraheavy\" elements with atomic numbers in the range Z=30 to 40. In addition, elemental energy spectra have now been measured over a significant fraction of two solar cycles, thereby enabling studies of the time dependence of the solar modulation of galactic cosmic rays.",
"doi": "10.22323/1.301.1089",
"publisher": "SISSA",
"publication_date": "2017-07"
},
{
"id": "authors:557tf-b1y27",
"collection": "authors",
"collection_id": "557tf-b1y27",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122926697",
"type": "book_section",
"title": "Capabilities and Performance of the High-Energy Energetic-Particles Instrument for the Parker Solar Probe Mission",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Burnham",
"given_name": "J. A.",
"clpid": "Burnham-J-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Crabill",
"given_name": "R. M.",
"clpid": "Crabill-R-M"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Hernandez",
"given_name": "L.",
"clpid": "Hernandez-L"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Klemic",
"given_name": "J.",
"clpid": "Klemic-J"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lopez",
"given_name": "S.",
"clpid": "Lopez-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Miyasaka",
"given_name": "H.",
"orcid": "0000-0002-8074-4186",
"clpid": "Miyasaka-Hiromasa"
},
{
"family_name": "Rankin",
"given_name": "J. S.",
"orcid": "0000-0002-8111-1444",
"clpid": "Rankin-J-S"
},
{
"family_name": "Riggans",
"given_name": "G.",
"clpid": "Riggans-G"
},
{
"family_name": "Rusert",
"given_name": "M. D.",
"clpid": "Rusert-M-D"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "White",
"given_name": "M. L.",
"clpid": "White-M-L"
}
],
"abstract": "NASA's Parker Solar Probe (PSP) spacecraft (formerly Solar Probe Plus) is scheduled for launch in July 2018 with a planned heliocentric orbit that will carry it on a series of close passes by the Sun with perihelion distances that eventually will get below 10 solar radii. Among other in-situ and imaging sensors, the PSP payload includes the two-instrument \"Integrated Science Investigation of the Sun\" suite, which will make coordinated measurements of energetic ions and electrons. The high-energy instrument (EPI-Hi), operating in the MeV energy range, consists of three detector-telescopes using silicon solid-state sensors for measuring composition, energy spectra, angular distributions, and time structure in solar energetic particle events. The expected performance of this instrument has been studied using accelerator calibrations, radioactive-source tests, and simulations. We present the EPI-Hi measurement capabilities drawing on these calibration data and simulation results for illustrations.",
"doi": "10.22323/1.301.0016",
"publisher": "SISSA",
"publication_date": "2017-07"
},
{
"id": "authors:0a850-j0f82",
"collection": "authors",
"collection_id": "0a850-j0f82",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-082135453",
"type": "monograph",
"title": "The Intensities of Cosmic Ray H and He Nuclei at ~250 MeV/nuc Measured by Voyagers 1 and 2 - Using these Intensities to Determine the Solar Modulation Parameter in the Inner Heliosphere and the Heliosheath Over a 40 Year Time Period",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-Nand"
}
],
"abstract": "We have determined the solar modulation potential, \u03a6, vs. time that is observed at Voyager 1 and 2 from measurements of the H and He nuclei intensities at a common energy of 250 MeVnuc. The H nuclei have a rigidity 0.7 GV, the He nuclei 1.4 GV. These measurements cover a 40 year time period, which includes almost 4 cycles of solar 11 year sunspot variations, throughout the inner heliosphere out to the HTS at distances of 95 AU and 85 AU, respectively at V1 and V2, and then beyond in the heliosheath. Inside the HTS the modulation potential vs. time curves at V1 and V2 show a very similar temporal structure to those observed at the Earth. During a later period of maximum solar modulation from 2000.0 to 2005.0 when V1 and V2 are in the outer heliosphere between 60-94 AU, the main temporal features of the modulation potential curves at all 3 locations match up with appropriate time delays at V1 and V2 if it is assumed that spatially coherent structures are moving outward past V1 and V2, with outward speeds of up to 700 Kms\u207b\u00b9. After 2004.0 V1 and V2 are at latitudes of +35\u00b0 and -30\u00b0 respectively, placing lower limits on the latitude extent of these structures. Beyond the HTS in the heliosheath the modulation potential slowly decreases at both spacecraft with only a weak evidence of the unusual modulation minimum observed at the Earth in 2009, for example. A sudden decrease of the modulation potential 50 MV for both H and He nuclei occurs at V1 just before the heliopause crossing at about 122 AU. This decrease has not yet been observed at V2, which is now at 113 AU and still observing a modulation potential 60 MV.",
"doi": "10.48550/arXiv.1706.02772",
"publisher": "arXiv",
"publication_date": "2017-06-08"
},
{
"id": "authors:hw75f-x3841",
"collection": "authors",
"collection_id": "hw75f-x3841",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140709-091502003",
"type": "article",
"title": "Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation",
"author": [
{
"family_name": "McComas",
"given_name": "D. J.",
"orcid": "0000-0001-6160-1158",
"clpid": "McComas-D-J"
},
{
"family_name": "Burnham",
"given_name": "J. A.",
"clpid": "Burnham-J-A"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Klemic",
"given_name": "J.",
"clpid": "Klemic-J"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Rankin",
"given_name": "J. S.",
"orcid": "0000-0002-8111-1444",
"clpid": "Rankin-J-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "The Integrated Science Investigation of the Sun (ISIS) is a complete science investigation on the Solar Probe Plus (SPP) mission, which flies to within nine solar radii of the Sun's surface. ISIS comprises a two-instrument suite to measure energetic particles over a very broad energy range, as well as coordinated management, science operations, data processing, and scientific analysis. Together, ISIS observations allow us to explore the mechanisms of energetic particles dynamics, including their: (1) Origins\u2014defining the seed populations and physical conditions necessary for energetic particle acceleration; (2) Acceleration\u2014determining the roles of shocks, reconnection, waves, and turbulence in accelerating energetic particles; and (3) Transport\u2014revealing how energetic particles propagate from the corona out into the heliosphere. The two ISIS Energetic Particle Instruments measure lower (EPI-Lo) and higher (EPI-Hi) energy particles. EPI-Lo measures ions and ion composition from \u223c20 keV/nucleon\u201315 MeV total energy and electrons from \u223c25\u20131000 keV. EPI-Hi measures ions from \u223c1\u2013200 MeV/nucleon and electrons from \u223c0.5\u20136 MeV. EPI-Lo comprises 80 tiny apertures with fields-of-view (FOVs) that sample over nearly a complete hemisphere, while EPI-Hi combines three telescopes that together provide five large-FOV apertures. ISIS observes continuously inside of 0.25 AU with a high data collection rate and burst data (EPI-Lo) coordinated with the rest of the SPP payload; outside of 0.25 AU, ISIS runs in low-rate science mode whenever feasible to capture as complete a record as possible of the solar energetic particle environment and provide calibration and continuity for measurements closer in to the Sun. The ISIS Science Operations Center plans and executes commanding, receives and analyzes all ISIS data, and coordinates science observations and analyses with the rest of the SPP science investigations. Together, ISIS' unique observations on SPP will enable the discovery, untangling, and understanding of the important physical processes that govern energetic particles in the innermost regions of our heliosphere, for the first time. This paper summarizes the ISIS investigation at the time of the SPP mission Preliminary Design Review in January 2014.",
"doi": "10.1007/s11214-014-0059-1",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2016-12",
"series_number": "1",
"volume": "204",
"issue": "1",
"pages": "187-256"
},
{
"id": "authors:sqqfe-61v61",
"collection": "authors",
"collection_id": "sqqfe-61v61",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160422-072602817",
"type": "article",
"title": "Observation of the ^(60)Fe nucleosynthesis-clock isotope in galactic cosmic rays",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "^(60)Fe is a radioactive isotope in cosmic rays that serves as a clock to infer an upper limit on the time between nucleosynthesis and acceleration. We have used the ACE-CRIS instrument to collect 3.55 \u00d7 10^5 iron nuclei, with energies ~195 to ~500 MeV/nucleon, of which we identify 15 ^(60)Fe nuclei. The ^(60)Fe/^(56)Fe source ratio is (7.5 \u00b1 2.9) \u00d7 10^(\u22125). The detection of supernova-produced ^(60)Fe in cosmic rays implies that the time required for acceleration and transport to Earth does not greatly exceed the ^(60)Fe half-life of 2.6 Myr and that the ^(60)Fe source distance does not greatly exceed the distance cosmic rays can diffuse over this time, \u2a8d 1 kpc. A natural place for ^(60)Fe origin is in nearby clusters of massive stars.",
"doi": "10.1126/science.aad6004",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "2016-05-06",
"series_number": "6286",
"volume": "352",
"issue": "6286",
"pages": "677-680"
},
{
"id": "authors:mrwcx-3pt37",
"collection": "authors",
"collection_id": "mrwcx-3pt37",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170223-134545862",
"type": "book_section",
"title": "Particle acceleration and reconnection in the solar wind",
"book_title": "SOLAR WIND 14: Proceedings of the Fourteenth International Solar Wind Conference",
"author": [
{
"family_name": "Zank",
"given_name": "G. P.",
"orcid": "0000-0002-4642-6192",
"clpid": "Zank-G-P"
},
{
"family_name": "Hunana",
"given_name": "P.",
"clpid": "Hunana-P"
},
{
"family_name": "Mostafavi",
"given_name": "P.",
"clpid": "Mostafavi-P"
},
{
"family_name": "le Roux",
"given_name": "J. A.",
"clpid": "Le-Roux-J-A"
},
{
"family_name": "Webb",
"given_name": "G. M.",
"clpid": "Webb-G-M"
},
{
"family_name": "Khabarova",
"given_name": "O.",
"clpid": "Khabarova-O"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Decker",
"given_name": "R. B.",
"clpid": "Decker-R-B"
}
],
"abstract": "An emerging paradigm for the dissipation of magnetic turbulence in the supersonic solar wind is via localized quasi-2D small-scale magnetic island reconnection processes. An advection-diffusion transport equation for a nearly isotropic particle distribution describes particle transport and energization in a region of interacting magnetic islands [1; 2]. The dominant charged particle energization processes are 1) the electric field induced by quasi-2D magnetic island merging, and 2) magnetic island contraction. The acceleration of charged particles in a \"sea of magnetic islands\" in a super-Alfv\u00e9nic flow, and the energization of particles by combined diffusive shock acceleration (DSA) and downstream magnetic island reconnection processes are discussed.",
"doi": "10.1063/1.4943848",
"isbn": "978-0-7354-1367-2",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2016-03-25",
"pages": "Art. No. 070011"
},
{
"id": "authors:kacpp-db347",
"collection": "authors",
"collection_id": "kacpp-db347",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160329-095104677",
"type": "book_section",
"title": "Solar energetic particle anisotropies and insights into particle transport",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Wang",
"given_name": "Linghua",
"clpid": "Wang-Linghua"
},
{
"family_name": "Bruno",
"given_name": "Roberto",
"clpid": "Bruno-R"
},
{
"family_name": "M\u00f6bius",
"given_name": "Eberhard",
"clpid": "M\u00f6bius-E"
},
{
"family_name": "Vourlidas",
"given_name": "Angelos",
"clpid": "Vourlidas-A"
},
{
"family_name": "Zank",
"given_name": "Gary",
"clpid": "Zank-G-P"
}
],
"abstract": "As solar energetic particles (SEPs) travel through interplanetary space, their pitch-angle distributions are shaped by the competing effects of magnetic focusing and scattering. Measurements of SEP anisotropies can therefore reveal information about interplanetary conditions such as magnetic field strength, topology, and turbulence levels at remote locations from the observer. Onboard each of the two STEREO spacecraft, the Low Energy Telescope (LET) measures pitch-angle distributions for protons and heavier ions up to iron at energies of about 2-12\u2005MeV/nucleon. Anisotropies observed using LET include bidirectional flows within interplanetary coronal mass ejections, sunward-flowing particles when STEREO was magnetically connected to the back side of a shock, and loss-cone distributions in which particles with large pitch angles underwent magnetic mirroring at an interplanetary field enhancement that was too weak to reflect particles with the smallest pitch angles. Unusual oscillations in the width of a beamed distribution at the onset of the 23 July 2012 SEP event were also observed and remain puzzling. We report LET anisotropy observations at both STEREO spacecraft and discuss their implications for SEP transport, focusing exclusively on the extreme event of 23 July 2012 in which a large variety of anisotropies were present at various times during the event.",
"doi": "10.1063/1.4943841",
"publisher": "American Institute of Physics",
"publication_date": "2016-03-22"
},
{
"id": "authors:chzt2-ykn38",
"collection": "authors",
"collection_id": "chzt2-ykn38",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160324-112710122",
"type": "article",
"title": "Diffusive Shock Acceleration and Reconnection Acceleration Processes",
"author": [
{
"family_name": "Zank",
"given_name": "G. P.",
"orcid": "0000-0002-4642-6192",
"clpid": "Zank-G-P"
},
{
"family_name": "Hunana",
"given_name": "P.",
"clpid": "Hunana-P"
},
{
"family_name": "Mostafavi",
"given_name": "P.",
"clpid": "Mostafavi-P"
},
{
"family_name": "Le Roux",
"given_name": "J. A.",
"clpid": "Le-Roux-J-A"
},
{
"family_name": "Li",
"given_name": "Gang",
"orcid": "0000-0001-9313-251X",
"clpid": "Li-Gang"
},
{
"family_name": "Webb",
"given_name": "G. M.",
"clpid": "Webb-G-M"
},
{
"family_name": "Khabarova",
"given_name": "O.",
"clpid": "Khabarova-O"
},
{
"family_name": "Cummings",
"given_name": "A.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E.",
"clpid": "Stone-E"
},
{
"family_name": "Decker",
"given_name": "R.",
"clpid": "Decker-R"
}
],
"abstract": "Shock waves, as shown by simulations and observations, can generate high levels of downstream vortical turbulence, including magnetic islands. We consider a combination of diffusive shock acceleration (DSA) and downstream magnetic-island-reconnection-related processes as an energization mechanism for charged particles. Observations of electron and ion distributions downstream of interplanetary shocks and the heliospheric termination shock (HTS) are frequently inconsistent with the predictions of classical DSA. We utilize a recently developed transport theory for charged particles propagating diffusively in a turbulent region filled with contracting and reconnecting plasmoids and small-scale current sheets. Particle energization associated with the anti-reconnection electric field, a consequence of magnetic island merging, and magnetic island contraction, are considered. For the former only, we find that (i) the spectrum is a hard power law in particle speed, and (ii) the downstream solution is constant. For downstream plasmoid contraction only, (i) the accelerated spectrum is a hard power law in particle speed; (ii) the particle intensity for a given energy peaks downstream of the shock, and the distance to the peak location increases with increasing particle energy, and (iii) the particle intensity amplification for a particular particle energy, f(x,c/c_0)/f(0,c/c_0), is not 1, as predicted by DSA, but increases with increasing particle energy. The general solution combines both the reconnection-induced electric field and plasmoid contraction. The observed energetic particle intensity profile observed by Voyager 2 downstream of the HTS appears to support a particle acceleration mechanism that combines both DSA and magnetic-island-reconnection-related processes.",
"doi": "10.1088/0004-637X/814/2/137",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-12-01",
"series_number": "2",
"volume": "814",
"issue": "2",
"pages": "Art. No. 137"
},
{
"id": "authors:ntq8e-m6777",
"collection": "authors",
"collection_id": "ntq8e-m6777",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151020-083336736",
"type": "article",
"title": "Precursors To Interstellar Shocks of Solar Origin",
"author": [
{
"family_name": "Gurnett",
"given_name": "D. A.",
"clpid": "Gurnett-D-A"
},
{
"family_name": "Kurth",
"given_name": "W. S.",
"clpid": "Kurth-W-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Decker",
"given_name": "R. B.",
"clpid": "Decker-R-B"
},
{
"family_name": "Ness",
"given_name": "N. F.",
"clpid": "Ness-N-F"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
}
],
"abstract": "On or about 2012 August 25, the Voyager 1 spacecraft crossed the heliopause into the nearby interstellar plasma. In the nearly three years that the spacecraft has been in interstellar space, three notable particle and field disturbances have been observed, each apparently associated with a shock wave propagating outward from the Sun. Here, we present a detailed analysis of the third and most impressive of these disturbances, with brief comparisons to the two previous events, both of which have been previously reported. The shock responsible for the third event was first detected on 2014 February 17 by the onset of narrowband radio emissions from the approaching shock, followed on 2014 May 13 by the abrupt appearance of intense electron plasma oscillations generated by electrons streaming outward ahead of the shock. Finally, the shock arrived on 2014 August 25, as indicated by a jump in the magnetic field strength and the plasma density. Various disturbances in the intensity and anisotropy of galactic cosmic rays were also observed ahead of the shock, some of which are believed to be caused by the reflection and acceleration of cosmic rays by the magnetic field jump at the shock, and/or by interactions with upstream plasma waves. Comparisons to the two previous weaker events show somewhat similar precursor effects, although differing in certain details. Many of these effects are very similar to those observed in the region called the \"foreshock\" that occurs upstream of planetary bow shocks, only on a vastly larger spatial scale.",
"doi": "10.1088/0004-637X/809/2/121",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-08-10",
"series_number": "2",
"volume": "809",
"issue": "2",
"pages": "Art. No. 121"
},
{
"id": "authors:62bqc-vh988",
"collection": "authors",
"collection_id": "62bqc-vh988",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180824-100033018",
"type": "book_section",
"title": "Cosmic rays beyond the boundary of the heliosphere",
"author": [
{
"family_name": "Florinski",
"given_name": "V.",
"orcid": "0000-0001-5485-2872",
"clpid": "Florinski-V"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "le Roux",
"given_name": "J. A.",
"clpid": "Le-Roux-J-A"
}
],
"abstract": "In August of 2012 the Voyager 1 space probe has left the solar-wind bubble of ionized gas we call the heliosphere and entered the denser and colder environment of the interstellar cloud surrounding the solar system. Energetic charged particles underwent dramatic changes past the heliopause: the heliospheric ions disappeared completely, while the galactic cosmic rays were for the first time measured in their unmodulated state. The interstellar medium turned out to be almost entirely devoid of turbulent magnetic fluctuations, therefore the transport of cosmic rays is governed by\na large-scale geometry of the magnetic field. We discuss observations of heliospheric ions, including\nanomalous cosmic rays, near the heliopause transition, and propose interpretations of the measured intensities and pitch-angle distributions based on gradient drift in a weakly nonuniform magnetic field. The heliopause transition appears to be permeated by magnetic flux tubes connected to the interstellar space and facilitating particle escape. These flux tubes may be a product of interchange instability driven by a plasma pressure gradient across the heliopause. The curvature of magnetic field lines and the anti-sunward gradient in plasma kinetic pressure provide conditions favorable for an interchange. The two flux tube crossings by the spacecraft allowed an indirect measurement of the plasma radial velocity near the heliopause.",
"doi": "10.22323/1.236.0214",
"publisher": "SISSA",
"publication_date": "2015-08"
},
{
"id": "authors:s2e6c-mey70",
"collection": "authors",
"collection_id": "s2e6c-mey70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122925525",
"type": "book_section",
"title": "Analysis of GCR Spectra and Composition Using Penetrating Particle Data from the CRIS Instrument on ACE",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The Cosmic Ray Isotope Spectrometer (CRIS) on NASA's Advanced Composition Explorer (ACE) spacecraft has been making precise measurements of cosmic-ray elemental and isotopic composition and energy spectra for nearly 18 years. This instrument uses the dE/dx versus total energy technique to identify nuclei that stop in thick stacks of silicon solid-state detectors and to measure their energy. The energy range covered for these stopping particles extends up to \u223c280 MeV/nuc for O and \u223c570 MeV/nuc for Fe. We have developed a new technique for identifying particles that penetrate the entire detector stack that relies on a combination of the total energy deposited in the stack and the change of dE/dx from the front to the back of the stack. This technique allows us to extend energy spectra for cosmic-ray elements to higher energies and can be used for bridging the energy gap between the CRIS stopping-particle spectra and measurements made in low-Earth orbit by instruments such as HEAO-C2, PAMELA, and AMS-02. We describe the technique for assigning atomic number and energy to penetrating particle events and discuss the corrections needed for deriving energy spectra from these data.",
"doi": "10.22323/1.236.0340",
"publisher": "SISSA",
"publication_date": "2015-08"
},
{
"id": "authors:82q84-pvn72",
"collection": "authors",
"collection_id": "82q84-pvn72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122924218",
"type": "book_section",
"title": "Voyager 1 Observations of Galactic Cosmic Rays in the Local Interstellar Medium: Energy Density and Ionization Rates",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-Nand"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "J\u00f3hannesson",
"given_name": "G.",
"clpid": "J\u00f3hannesson-G"
},
{
"family_name": "Moskalenko",
"given_name": "I. V.",
"clpid": "Moskalenko-I-V"
},
{
"family_name": "Orlando",
"given_name": "E.",
"clpid": "Orlando-E"
},
{
"family_name": "Porter",
"given_name": "T. A.",
"clpid": "Porter-T-A"
}
],
"abstract": "Voyager 1 (V1) has been in the local interstellar medium (LISM) since August, 2012. We present the galactic cosmic-ray (GCR) energy spectra of most elements from H through Ni, and also of electrons, for a period exceeding two years. The V1 energy spectra define the newly-revealed, low-energy part of the interstellar spectra of nuclei down to ~3 MeV nuc^(-1) and of electrons down to ~5 MeV. We use a leaky-box model and three GALPROP models of the local interstellar spectra of nuclei, constrained by the V1 observations at low energies and by observations at 1 AU from other missions at higher energies, to estimate the cosmic-ray energy density and the ionization rate of atomic H in the local interstellar medium by nuclei above 3 MeV nuc ^(-1). We use a model of the interstellar electron spectrum that approximately matches the V1 observations to derive the electron contributions to the cosmic-ray energy density and the ionization rate of atomic H above 3 MeV. We find that the total cosmic-ray energy density is in the range 0.82-0.97 eV cm^(-3), which includes a contribution of 0.023 eV cm^(-3) from electrons. We find the cosmic-ray ionization rate of atomic H to be in the range 1.45-1.58 X 10^-17) s^(-1), which is a factor of more than 10 below the cosmic-ray ionization rate in diffuse interstellar clouds based on astrochemistry methods. We discuss possible reasons for this difference.",
"doi": "10.22323/1.236.0318",
"publisher": "SISSA",
"publication_date": "2015-08"
},
{
"id": "authors:gnrmp-0aa81",
"collection": "authors",
"collection_id": "gnrmp-0aa81",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180910-131322207",
"type": "book_section",
"title": "Insights Into Particle Transport Obtained from Solar Energetic Particle Anisotropies",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Solar energetic particle (SEP) pitch-angle distributions are shaped by the competing effects of magnetic focusing and scattering as the particles travel through interplanetary space. Therefore, measurements of SEP anisotropies provide insight into particle transport and can probe interplanetary conditions at remote locations from the observer. The Low Energy Telescopes (LETs) onboard the twin STEREO spacecraft measure pitch-angle distributions for protons and heavier ions at energies of about 2-12 MeV/nucleon. Using these instruments, we have observed a wide variety of SEP anisotropies, such as bidirectional flows within interplanetary coronal mass ejections, sunward-flowing particles when the spacecraft was magnetically connected to the back side of a distant shock, and loss-cone distributions in which particles with large pitch angles magnetically mirror at an interplanetary field enhancement that is too weak to reflect particles with the smallest pitch angles. One of the more puzzling observations is unusual oscillations on a timescale of several minutes in the width of a beamed distribution at the onset of the very large 23 July 2012 SEP event. We report LET anisotropy observations at both STEREO spacecraft during the extreme event of 23 July 2012, in which a large range of anisotropies were observed at various times during the event, and discuss their implications for SEP transport.",
"doi": "10.22323/1.236.0072",
"publisher": "SISSA",
"publication_date": "2015-08"
},
{
"id": "authors:d9c7s-d6r21",
"collection": "authors",
"collection_id": "d9c7s-d6r21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122925213",
"type": "book_section",
"title": "Inferred Ionic Charge States for Solar Energetic Particle Events from 2012-2015 with ACE and STEREO",
"author": [
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Sollitt",
"given_name": "L. S.",
"clpid": "Sollitt-L-S"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "Mean ionic charge states for SEP events can reflect source temperatures, stripping during acceleration and transport, and the composition of source material. Multi-spacecraft measurements of mean ionic charge states for single SEP events can also demonstrate longitudinal dependence depending on seed particle composition or acceleration conditions. in previous studies, we calculated inferred high-energy ionic charge states for SEP events. The analysis method fits the energy dependence of decay times for each element in SEP events, combined with charge-to-mass ratios relative to a calibration element, and derives mean charge state estimates for elements from O to Fe. Previously, we applied the method using ACE and STEREO data to SEP events through the beginning of 2012, in order to elucidate evidence on seed populations or longitudinal variations with charge state for single SEP events, with varying results. In this paper, we continue applying the method to new SEP events from 2012 to 2015 in the ACE and STEREO data. With the three spacecraft widely spread apart during this time period, there are fewer single SEP events with multi-spacecraft data, but the wide spacing allows more SEP candidate events to be considered, separately, than would be available with just a single spacecraft. Our new results for two SEP events continue to be consistent with observed correlation between Q(Fe) and Fe/O in previous events.",
"doi": "10.22323/1.236.0107",
"publisher": "SISSA",
"publication_date": "2015-08"
},
{
"id": "authors:ww5ab-hta10",
"collection": "authors",
"collection_id": "ww5ab-hta10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180910-131321786",
"type": "book_section",
"title": "Elemental Abundances of Ultra-Heavy GCRs measured by SuperTIGER and ACE-CRIS and the Origin of Galactic Cosmic Rays",
"author": [
{
"family_name": "Hams",
"given_name": "T.",
"clpid": "Hams-T"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Brandt",
"given_name": "T. J.",
"orcid": "0000-0003-4087-1786",
"clpid": "Brandt-T-J"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Dowkontt",
"given_name": "P. F.",
"clpid": "Dowkontt-P-F"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Krizmanic",
"given_name": "J. F.",
"clpid": "Krizmanic-J-F"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Link",
"given_name": "J. T.",
"clpid": "Link-J-T"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mitchell",
"given_name": "J. W.",
"clpid": "Mitchell-J-W"
},
{
"family_name": "Murphy",
"given_name": "R. P.",
"clpid": "Murphy-R-P"
},
{
"family_name": "Rauch",
"given_name": "B. F.",
"clpid": "Rauch-B-F"
},
{
"family_name": "Sakai",
"given_name": "K.",
"clpid": "Sakai-Kenichi"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-Makoto"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Waddington",
"given_name": "C. J.",
"clpid": "Waddington-C-J"
},
{
"family_name": "Ward",
"given_name": "J. E.",
"clpid": "Ward-J-E"
},
{
"family_name": "Westphal",
"given_name": "A. J.",
"clpid": "Westphal-A-J"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "The Super Trans-Iron Galactic Element Recorder (SuperTIGER) long-duration balloon instrument and the Cosmic Ray Isotope Spectrometer (CRIS) on the NASA Advanced Composition Explorer (ACE) satellite have measured the abundances of galactic cosmic-ray elements from _(10)Ne to _(40)Zr with high statistics and single-element resolution. SuperTIGER launched from Williams Field, McMurdo Station, Antarctica, on December 8, 2012, flying for a record 55 days. During that flight we detected \u223c1,300 nuclei with atomic number Z \u2265 30. The resolution in charge (Z) of SuperTIGER is excellent, with \u03c3_Z \u2248 0.16 c.u. at _(26)Fe. SuperTIGER is sensitive to nuclei with energy at the top of the atmosphere of E > 0.8 GeV/nucleon. The instrument has now been recovered and preparations are underway for its next flight. ACE/CRIS has been taking data in space for more than 17 years since launch in 1997, has collected \u223c625 nuclei with atomic number Z \u2265 30, and shows excellent resolution with clear separation between the charges for 30 \u2264 Z \u2264 40. ACE/CRIS is sensitive to nuclei in the energy range 150 \u2264 E \u2264 600 MeV/nucleon. Preliminary results from the balloon-borne SuperTIGER show good agreement with ACE measurements in space, validating our corrections to SuperTIGER abundances for nuclear interactions in the atmosphere. The results from these experiments will be discussed in the context of the OB association model for the origin of galactic cosmic rays. Future missions to measure elemental abundances to higher Z, the SuperTIGER-II LDB instrument and the orbiting Heavy Nuclei eXplorer (HNX) mission, will also be discussed.",
"doi": "10.22323/1.236.0038",
"publisher": "SISSA",
"publication_date": "2015-08"
},
{
"id": "authors:n5x3q-5qz02",
"collection": "authors",
"collection_id": "n5x3q-5qz02",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122925311",
"type": "book_section",
"title": "Observation of ^(60)Fe in the Galactic Cosmic Rays",
"author": [
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "The Cosmic Ray Isotope Spectrometer (CRIS) on the ACE spacecraft has been measuring the isotopic composition of Galactic Cosmic Rays (GCRs) since August 1997. Using selected data from the past seventeen years, we have a set of 2.95 x 10^5 ^(56)Fe nuclei in the energy interval ~240 to ~470 MeV/nucleon with excellent mass resolution characterized by \u03c3 = 0.24 amu. In this data set we have detected fifteen well resolved ^(60)Fe nuclei. ^(60)Fe is \u03b2^- unstable with a half-life of 2.6 million years. The detection of these radioactive nuclei permits us to set an upper limit of a few million years on the time between nucleosynthesis of these nuclei and their acceleration to cosmic-ray energies. A lower limit of ~10^5 years was established by the CRIS observation that the electron-capture isotope ^(59)Ni is essentially absent in the GCRs. These two limits bracket the nucleosynthesis-to-acceleration time to a range that is consistent with the emerging evidence that the bulk of GCRs are accelerated in associations of massive stars (OB associations).",
"doi": "10.22323/1.236.0275",
"publisher": "SISSA",
"publication_date": "2015-08"
},
{
"id": "authors:xmae6-abw36",
"collection": "authors",
"collection_id": "xmae6-abw36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122925629",
"type": "book_section",
"title": "The Longitudinal Distribution of Solar Energetic Particles",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Richardson",
"given_name": "I. G.",
"orcid": "0000-0002-3855-3634",
"clpid": "Richardson-I-G"
},
{
"family_name": "Cane",
"given_name": "H. V.",
"clpid": "Cane-H-V"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "Using observations from the High Energy Telescopes (HETs) on STEREO A and B and similar observations from SoHO, near-Earth, we have identified ~250 individual solar energetic particle events that include >14 MeV protons since the beginning of the STEREO mission [1]. Between the end of December 2009, when the STEREO A and B spacecraft were, respectively, ahead and behind Earth by ~ 65\u00b0 in ecliptic longitude, and the end of December 2013, 43 different events were clearly detected at all three locations. The observed intensities of such an event are usually assumed to be Gaussian distributed as a function of the longitudes of the Parker Spiral footpoints at the Sun for each observer. This neglects the fact that the interplanetary magnetic field may have large deviations from Parker Spirals, e.g. due to coronal mass ejections from\nprior events. Nonetheless, we have fit Gaussians to the peak intensities observed simultaneously at three spacecraft for all 43 events. The Gaussian peak intensity is poorly correlated with the corresponding CME speed and the FWHM is uncorrelated with the CME speed. Surprisingly, however, there appear to be distinctly non-random variations of the FWHM values from event to event.",
"doi": "10.22323/1.236.0104",
"publisher": "SISSA",
"publication_date": "2015-08"
},
{
"id": "authors:7fcww-ftx52",
"collection": "authors",
"collection_id": "7fcww-ftx52",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150604-140432982",
"type": "article",
"title": "Spectral Evolution of Anomalous Cosmic Rays at Voyager 1 beyond the Termination Shock",
"author": [
{
"family_name": "Senanayake",
"given_name": "U. K.",
"clpid": "Senanayake-U-K"
},
{
"family_name": "Florinski",
"given_name": "V.",
"orcid": "0000-0001-5485-2872",
"clpid": "Florinski-V"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "When the Voyager 1 spacecraft crossed the termination shock (TS) on 2004 December 16, the energy spectra of anomalous cosmic rays (ACRs) could not have been produced by steady-state diffusive shock acceleration. However, over the next few years, in the declining phase of the solar cycle, the spectra began to evolve into the expected power-law profile. Observations at the shock led to a broad range of alternative theories for ACR acceleration. In spite of that, in this work we show that the observations could be explained by assuming ACRs are accelerated at the TS. In this paper, we propose that the solar cycle had an important effect on the unrolling of the spectra in the heliosheath. To investigate the spectral evolution of ACRs, a magnetohydrodynamic background model with stationary solar-wind inner boundary conditions was used to model the transport of helium and oxygen ions. We used a backward-in-time stochastic integration technique where phase-space trajectories are integrated until the so-called \"injection energy\" is reached. Our simulation results were compared with Voyager 1 observations using three different diffusion models. It is shown that the spectral evolution of ACRs in the heliosheath at Voyager 1 could be explained by an increase in the source strength and an enhancement in diffusion as a result of a decrease of the turbulent correlation length in the declining phase of the solar cycle. At the same time, drift effects seem to have had a smaller effect on the evolution of the spectra.",
"doi": "10.1088/0004-637X/804/1/12",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-05-01",
"series_number": "1",
"volume": "804",
"issue": "1",
"pages": "Art. No. 12"
},
{
"id": "authors:a96e5-s3z10",
"collection": "authors",
"collection_id": "a96e5-s3z10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150518-085218576",
"type": "article",
"title": "Energetic Particle Anisotropies at the Heliospheric Boundary. II. Transient Features and Rigidity Dependence",
"author": [
{
"family_name": "Florinski",
"given_name": "V.",
"orcid": "0000-0001-5485-2872",
"clpid": "Florinski-V"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Le Roux",
"given_name": "J. A.",
"clpid": "Le-Roux-J-A"
}
],
"abstract": "In the preceding paper, we showed that large second-order anisotropies of heliospheric ions measured by the Voyager 1 space probe during the August 2012 boundary crossing event could be explained by a magnetic shear across the heliopause preventing particles streaming along the magnetic field from escaping the inner heliosheath. According to Stone et al., the penetration distance of heliospheric ions into the outer heliosheath had a strong dependence on the particle's Larmor radius. By comparing hydrogen, helium, and oxygen ions with the same energy per nucleon, these authors argued that this effect must be attributed to larger cyclotron radii of heavier species rather than differences in velocity. We propose that gradient drift in a nonuniform magnetic field was the cause of both the large second-order anisotropies and the spatial differentiation based on the ion's rigidity. A latitudinal gradient of magnetic field strength of about 10% per AU between 2012.7 and 2012.9 could have provided drift motion sufficient to match both LECP and CRS Voyager 1 observations. We explain the transient intensity dropout observed prior to the heliocliff using flux tube structures embedded in the heliosheath and magnetically connected to interstellar space. Finally, this paper reports a new indirect measurement of the plasma radial velocity at the heliopause on the basis of the time difference between two cosmic-ray telescopes measuring the same intensity dropout.",
"doi": "10.1088/0004-637X/803/1/47",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-04-10",
"series_number": "1",
"volume": "803",
"issue": "1",
"pages": "Art. No. 47"
},
{
"id": "authors:yya6h-gfp31",
"collection": "authors",
"collection_id": "yya6h-gfp31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130725-143748629",
"type": "article",
"title": "Voyager 1 Observes Low-Energy Galactic Cosmic Rays in a Region Depleted of Heliospheric Ions",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "On 25 August 2012, Voyager 1 was at 122 astronomical units when the steady intensity of low-energy ions it had observed for the previous 6 years suddenly dropped for a third time and soon completely disappeared as the ions streamed away into interstellar space. Although the magnetic field observations indicate that Voyager 1 remained inside the heliosphere, the intensity of cosmic ray nuclei from outside the heliosphere abruptly increased. We report the spectra of galactic cosmic rays down to ~3 \u00d7 10^6 electron volts per nucleon, revealing H and He energy spectra with broad peaks from 10 \u00d7 10^6 to 40 \u00d7 10^6 electron volts per nucleon and an increasing galactic cosmic-ray electron intensity down to ~10 \u00d7 10^6 electron volts.",
"doi": "10.1126/science.1236408",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "2013-07-12",
"series_number": "6142",
"volume": "341",
"issue": "6142",
"pages": "150-153"
},
{
"id": "authors:qqgnw-p8m74",
"collection": "authors",
"collection_id": "qqgnw-p8m74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130725-072008737",
"type": "article",
"title": "Galactic Cosmic-Ray Energy Spectra and Composition during the 2009-2010 Solar Minimum Period",
"author": [
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "We report new measurements of the elemental energy spectra and composition of galactic cosmic rays during the 2009-2010 solar minimum period using observations from the Cosmic Ray Isotope Spectrometer (CRIS) onboard the Advanced Composition Explorer. This period of time exhibited record-setting cosmic-ray intensities and very low levels of solar activity. Results are given for particles with nuclear charge 5 \u2264 Z \u2264 28 in the energy range ~50-550 MeV nucleon^(\u20131). Several recent improvements have been made to the earlier CRIS data analysis, and therefore updates of our previous observations for the 1997-1998 solar minimum and 2001-2003 solar maximum are also given here. For most species, the reported intensities changed by less than ~7%, and the relative abundances changed by less than ~4%. Compared with the 1997-1998 solar minimum relative abundances, the 2009-2010 abundances differ by less than 2\u03c3, with a trend of fewer secondary species observed in the more recent time period. The new 2009-2010 data are also compared with results of a simple \"leaky-box\" galactic transport model combined with a spherically symmetric solar modulation model. We demonstrate that this model is able to give reasonable fits to the energy spectra and the secondary-to-primary ratios B/C and (Sc+Ti+V)/Fe. These results are also shown to be comparable to a GALPROP numerical model that includes the effects of diffusive reacceleration in the interstellar medium.",
"doi": "10.1088/0004-637X/770/2/117",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2013-06-20",
"series_number": "2",
"volume": "770",
"issue": "2",
"pages": "Art. No. 117"
},
{
"id": "authors:k90rj-5sd35",
"collection": "authors",
"collection_id": "k90rj-5sd35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-083853990",
"type": "article",
"title": "Anomalous and Galactic Cosmic Rays at 1 AU During the Cycle 23/24 Solar Minimum",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "Anomalous cosmic ray (ACR) intensities at 1 AU at solar minimum generally track galactic cosmic ray (GCR) intensities such as those measured by neutron monitors, albeit with differences between solar polarity cycles. The unusual cycle 23/24 solar minimum was long-lasting with very low sunspot numbers and significantly reduced interplanetary magnetic field strength and solar wind dynamic pressure and turbulence, but also featured a heliospheric current sheet tilt that remained high for an extended period. Peak ACR intensities did not recover to the maximum values reached during the last two A>0 solar minima and just barely reached the last A<0 levels. However, GCR intensities in 2009 (neutron monitor rates and also at \u223c200 MeV/nucleon) were the highest recorded during the last 50 years, indicating their intensities were not as heavily modulated during their transport from the outer heliosphere. This unexpected difference in the behavior of ACRs and GCRs remains unexplained, but suggests that either the ACR source intensity may have weakened since the last A<0 epoch, or perhaps that ACR intensities at 1 AU in the ecliptic may be more sensitive than GCRs to the higher tilt angle. This seems plausible if the ACR source intensity is greater at low latitudes during A<0 cycles, while the GCR distribution at the heliospheric boundary is more uniform in latitude. Shortly after an abrupt increase in the current sheet tilt angle in late 2009, both ACR and GCR intensities showed dramatic decreases, marking the end of solar minimum modulation conditions for this cycle.",
"doi": "10.1007/s11214-011-9772-1",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2013-06",
"series_number": "1-4",
"volume": "176",
"issue": "1-4",
"pages": "253-263"
},
{
"id": "authors:w4hm9-8ms85",
"collection": "authors",
"collection_id": "w4hm9-8ms85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160420-130923910",
"type": "book_section",
"title": "Galactic cosmic rays in the distant heliosphere",
"book_title": "Centenary Symposium 2012: Discovery of Cosmic Rays",
"author": [
{
"family_name": "McDonald",
"given_name": "Frank B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"contributor": [
{
"family_name": "Ormes",
"given_name": "J. F.",
"clpid": "Ormes-J-F"
}
],
"abstract": "The small flotilla of spacecraft: Pioneers 10 and 11 and Voyagers 1 and 2 (V1 and V2) that have traveled from 1 AU to the distant heliosphere continue the quest of Victor Hess to understand the nature of this radiation that comes to us from beyond the confines of our solar system. At this time V1 and V2 are traveling deeper into the heliosheath and approaching its outer boundary - the heliopause. In the heliosheath the intensity of 2.5 - 60 MeV GCR electrons has risen significantly above detector background levels and provides an important new diagnostic tool for exploring cosmic ray transport in this previously unexplored region of space. Over the past seven months the intensity of GCR ions and electrons at V1 have remained constant after a steady, 5.5 year exponential increase whose rate varied with particle species. Is this an indication that V1 is approaching the heliopause?",
"doi": "10.1063/1.4792545",
"isbn": "978-0-7354-1137-1",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2013-02-07",
"pages": "85-88"
},
{
"id": "authors:6aqr9-6vz12",
"collection": "authors",
"collection_id": "6aqr9-6vz12",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130226-134144383",
"type": "book_section",
"title": "Anomalous Cosmic Rays",
"book_title": "Centenary Symposium 2012: Discovery of Cosmic Rays",
"author": [
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Ormes",
"given_name": "Jonathan F.",
"clpid": "Ormes-J-F"
}
],
"abstract": "Anomalous cosmic rays (ACRs) first started showing up in observations 40 years ago. Within a few years a paradigm was developed to explain their origin: they begin their life as interstellar neutral atoms that drift into the heliosphere, become singly ionized by chargeexchange with a solar wind ion or by photoionization, are picked up by the expanding solar wind, and accelerated to the observed energies by diffusive shock acceleration at the solar wind termination shock. This paradigm became widely accepted and withstood the tests of further observations until 16 December 2004, when Voyager 1 crossed the termination shock and didn't find their source. In August 2007, Voyager 2 crossed the termination shock and also did not find the source location of ACRs. Clearly, the source location was not at the termination shock where the two Voyagers crossed. Alternative models have been proposed with acceleration elsewhere on the shock or by other acceleration processes in the heliosheath. We discuss the latest observations of ACRs from the Voyager spacecraft and hopefully shed more light on this ongoing puzzle.",
"doi": "10.1063/1.4792547",
"isbn": "978-0-7354-1137-1",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2013-02-07",
"pages": "97-101"
},
{
"id": "authors:x23bh-srn28",
"collection": "authors",
"collection_id": "x23bh-srn28",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130625-131632943",
"type": "book_section",
"title": "A survey of anisotropic energetic particle flows observed by STEREO",
"book_title": "Solar Wind 13: Proceedings of the Thirteenth International Solar Wind Conference",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Dotson",
"given_name": "B.",
"clpid": "Dotson-B"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Zank",
"given_name": "Gary P.",
"clpid": "Zank-G-P"
},
{
"family_name": "Borovsky",
"given_name": "Joe",
"clpid": "Borovsky-J"
},
{
"family_name": "Bruno",
"given_name": "Roberto",
"clpid": "Bruno-R"
},
{
"family_name": "Cirtain",
"given_name": "Jonathan",
"clpid": "Cirtain-J"
},
{
"family_name": "Cranmer",
"given_name": "Steve",
"clpid": "Cranmer-S"
},
{
"family_name": "Elliott",
"given_name": "Heather",
"clpid": "Elliott-H"
},
{
"family_name": "Giacalone",
"given_name": "Joe",
"clpid": "Giacalone-J"
},
{
"family_name": "Gonzalez",
"given_name": "Walter",
"clpid": "Gonzalez-W"
},
{
"family_name": "Li",
"given_name": "Gang",
"clpid": "Li-Gang"
},
{
"family_name": "Marsch",
"given_name": "Eckart",
"clpid": "Marsch-E"
},
{
"family_name": "Moebius",
"given_name": "Eberhard",
"clpid": "Moebius-E"
},
{
"family_name": "Pogorelov",
"given_name": "Nick",
"clpid": "Pogorelov-P"
},
{
"family_name": "Spann",
"given_name": "Jim",
"clpid": "Spann-J"
},
{
"family_name": "Verkhoglyadova",
"given_name": "Olga",
"clpid": "Verkhoglyadova-O"
}
],
"abstract": "The Low Energy Telescopes (LETs) onboard the twin STEREO spacecraft have been measuring the anisotropies of energetic particles since before the beginning of solar cycle 24. Large unidirectional anisotropies often appear at the onset of magnetically well-connected solar energetic particle (SEP) events, suggesting beamed particles with relatively little scattering. Also, long-lasting bidirectional flows are seen during the decay phase of several SEP events. Some of these instances appear to be within interplanetary coronal mass ejections (ICMEs), as indicated by characteristics such as magnetic field rotations or bidirectional suprathermal electrons. We present preliminary findings from a survey of LET proton anisotropy observations, which illustrate that bidirectional flows appear more likely to come from directions far from the nominal Parker spiral direction than do unidirectional beams, consistent with previous studies. Individual cases that show unusual intensity depletions perpendicular to the magnetic field or pitch angle distributions otherwise indicative of magnetic mirroring are presented in more detail.",
"doi": "10.1063/1.4811029",
"isbn": "978-0-7354-1163-0",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2013",
"pages": "227-230"
},
{
"id": "authors:xrp58-d7449",
"collection": "authors",
"collection_id": "xrp58-d7449",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-084404748",
"type": "monograph",
"title": "At Voyager 1 Starting on about August 25, 2012 at a Distance of 121.7 AU From the Sun, a Sudden Disappearance of Anomalous Cosmic Rays and an Unusually Large Sudden Increase of Galactic Cosmic Ray H and He Nuclei and Electron Occurred",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-Nand"
}
],
"abstract": "At the Voyager 1 spacecraft in the outer heliosphere, after a series of complex intensity changes starting at about May 8th, the intensities of both anomalous cosmic rays (ACR) and galactic cosmic rays (GCR) changed suddenly and decisively on August 25th (121.7 AU from the Sun). The ACR started the intensity decrease with an initial e-folding rate of intensity decrease of ~1 day. Within a matter of a few days, the intensity of 1.9-2.7 MeV protons and helium nuclei had decreased to less than 0.1 of their previous value and after a few weeks, corresponding to the outward movement of V1 by ~0.1 AU, these intensities had decreased by factors of at least 300-500 and are now lower than most estimates of the GCR spectrum for these lower energies and also at higher energies. The decrease was accompanied by large rigidity dependent anisotropies in addition to the extraordinary rapidity of the intensity changes. Also on August 25th the GCR protons, helium and heavier nuclei as well as electrons increased suddenly with the intensities of electrons reaching levels ~30-50% higher than observed just one day earlier. This increase for GCR occurred over ~1 day for the lowest rigidity electrons, and several days for the higher rigidity nuclei of rigidity ~0.5-1.0 GV. After reaching these higher levels the intensities of the GCR of all energies from 2 to 400 MeV have remained essentially constant with intensity levels and spectra that may represent the local GCR. These intensity changes will be presented in more detail in this, and future articles, as this story unfolds.",
"doi": "10.48550/arXiv.1212.0883",
"publisher": "arXiv",
"publication_date": "2012-12-04"
},
{
"id": "authors:a4cjf-bfp18",
"collection": "authors",
"collection_id": "a4cjf-bfp18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121207-133222594",
"type": "article",
"title": "Large Proton Anisotropies in the 18 August 2010 Solar Particle Event",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The solar particle event observed at STEREO Ahead on 18 August 2010 displayed a rich variety of behavior in the particle anisotropies. Sectored rates measured by the Low Energy Telescope (LET) on STEREO showed very large bidirectional anisotropies in 4\u2009\u2013\u20096 MeV protons for the first \u223c\u200917 hours of the event while inside a magnetic cloud, with intensities along the field direction several hundred to nearly 1000 times greater than those perpendicular to the field. At the trailing end of the cloud, the protons became isotropic and their spectrum hardened slightly, while the He/H abundance ratio plunged by a factor of approximately four for about four hours. Associated with the arrival of a shock on 20 August was a series of brief (<\u200910 minute duration) intensity increases (commonly called \"shock spikes\") with relatively narrow angular distributions (\u223c\u200945\u2218 FWHM), followed by an abrupt decrease in particle intensities at the shock itself and a reversal of the proton flow to a direction toward the Sun and away from the receding shock. We discuss the STEREO/LET observations of this interesting event in the context of other observations reported in the literature.",
"doi": "10.1007/s11207-012-0018-5",
"issn": "0038-0938",
"publisher": "Springer",
"publication": "Solar Physics",
"publication_date": "2012-11",
"series_number": "1",
"volume": "281",
"issue": "1",
"pages": "301-318"
},
{
"id": "authors:v2q0q-thh59",
"collection": "authors",
"collection_id": "v2q0q-thh59",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-090030437",
"type": "monograph",
"title": "Large periodic time variations of termination shock particles between ~0.5-20 mev and 6-14 mev electrons measured by the crs experiment on Voyager 2 as it crossed into the heliosheath in 2007: An example of freshly accelerated cosmic rays?",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Intriligator",
"given_name": "D. S.",
"clpid": "Intriligator-D-S"
},
{
"family_name": "Higbie",
"given_name": "P. R.",
"clpid": "Higbie-P-R"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-Nand"
}
],
"abstract": "We have examined features in the structure of the heliosheath using the fine scale time variations of termination shock particles (TSP) between ~0.5 - 20 MeV and electrons between 2.5-14 MeV measured by the CRS instrument as the V2 spacecraft crossed the heliospheric termination shock in 2007. The very disturbed heliosheath at V2 is particularly noteworthy for strong periodic intensity variations of the TSP just after V2 crossed the termination shock (2007.66) reaching a maximum between 2007.75 and 2008.0. A series of 42/21 day periodicities was observed at V2 along with spectral changes of low energy TSP and the acceleration of 6-14 MeV electrons. Evidence is presented for the acceleration of TSP and electrons at the times of the 42/21 day periodicities just after V2 crossed the HTS. Spectra for TSP between 2-20 MeV and electrons between 2.5-14 MeV are derived for three time periods including the time of the HTS crossing. The energy spectra of TSP and electrons at these times of intensity peaks are very similar above ~3 MeV, with exponents of a power law spectrum between -3.0 and -3.6. The ratio of TSP intensities to electron intensities at the same energy is ~500. The electron intensity peaks and minima are generally out of phase with those of nuclei by ~1/2 of a 42 day cycle. These charge dependent intensity differences and the large periodic intensity changes could provide new clues as to a possible acceleration mechanism.",
"doi": "10.48550/arXiv.1208.2982",
"publisher": "arXiv",
"publication_date": "2012-08-14"
},
{
"id": "authors:4266a-vj606",
"collection": "authors",
"collection_id": "4266a-vj606",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120502-145049365",
"type": "article",
"title": "Sudden intensity increases and radial gradient changes of cosmic ray MeV electrons and protons observed at Voyager 1 beyond 111 AU in the heliosheath",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"abstract": "Voyager 1 has entered regions of different propagation conditions for energetic cosmic rays in the outer heliosheath at a distance of about 111 AU from the Sun. The low energy 6\u201314 MeV galactic electron intensity increased by ~20% over a time period \u226410 days and the electron radial intensity gradient abruptly decreased from \u223c19%/AU to \u223c8%/AU at 2009.7 at a radial distance of 111.2 AU. At about 2011.2 at a distance of 116.6 AU a second abrupt intensity increase of \u223c25% was observed for electrons. After the second sudden electron increase the radial intensity gradient increased to 18%/AU. This large positive gradient and the \u223c13 day periodic variations of >200 MeV particles observed near the end of 2011 indicate that V1 is still within the overall heliospheric modulating region. The implications of these results regarding the proximity of the heliopause are discussed.",
"doi": "10.1029/2012GL051171",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "2012-03-28",
"series_number": "6",
"volume": "39",
"issue": "6",
"pages": "Art. No. L06107"
},
{
"id": "authors:2j69t-cex68",
"collection": "authors",
"collection_id": "2j69t-cex68",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-101907790",
"type": "monograph",
"title": "20-125 MeV/nuc cosmic ray carbon nuclei intensities between 2004-2010 in solar cycle #23 as measured near the earth, at voyager 2 and also in the heliosheath at voyager 1 - modulation in a two zone heliospehre",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Higbie",
"given_name": "P. R.",
"clpid": "Higbie-P-R"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
}
],
"abstract": "The recovery of cosmic ray Carbon nuclei of energy ~20-125 MeV/nuc in solar cycle #23 from 2004 to 2010 has been followed at three locations, near the Earth using ACE data and at V2 between 74-92 AU and also at V1 beyond the heliospheric termination shock at between 91-113 AU. To describe the observed intensity changes and to predict the absolute intensities measured at all three locations we have used a simple spherically symmetric (no drift) two-zone heliospheric transport model with specific values for the diffusion coefficient in both the inner and outer zones. The diffusion coefficient in the outer zone is determined to be ~5-10 times smaller than that in the inner zone out to 90 AU. For both V1 and V2 the calculated C nuclei intensities agree within an average of \u00b110% with the observed intensities. Because of this agreement between V1 and V2 observations and predictions there is no need to invoke an asymmetrical squashed heliosphere or other effects to explain the V2 intensities relative to V1 as is the case for He nuclei. The combination of the diffusion parameters used in this model and the interstellar spectrum give an unusually low overall solar modulation parameter \u03a6 = 250 MV to describe the Carbon intensities observed at the Earth in 2009. At all times both the observed and calculated spectra are very closely ~ E^(1.0) as would be expected in the adiabatic energy loss regime of solar modulation.",
"doi": "10.48550/arXiv.1202.2081",
"publisher": "arXiv",
"publication_date": "2012-02-09"
},
{
"id": "authors:qvpcm-1jj49",
"collection": "authors",
"collection_id": "qvpcm-1jj49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120529-081329347",
"type": "book_section",
"title": "Observations of the longitudinal spread of solar energetic particle events in solar cycle 24",
"book_title": "Physics of the heliosphere: a 10 year retrospective",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Haggerty",
"given_name": "D. K.",
"orcid": "0000-0001-6395-8943",
"clpid": "Haggerty-D-K"
},
{
"family_name": "Gomez-Herrero",
"given_name": "R.",
"clpid": "Gomez-Herrero-R"
},
{
"family_name": "Bucik",
"given_name": "R.",
"clpid": "Bucik-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Korth",
"given_name": "A.",
"clpid": "Korth-A"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mall",
"given_name": "U.",
"clpid": "Mall-U"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Heerikhuisen",
"given_name": "Jacob",
"clpid": "Heerikhuisen-J"
}
],
"abstract": "With the twin STEREO spacecraft, significantly separated from L1-based satellites such as ACE, simultaneous multi-point measurements of solar energetic particle (SEP) events can be made for H-Fe ions from a few hundred keV/nuc to over 100 MeV/nuc and for electrons from tens to hundreds of keV. These observations allow studies of the longitudinal characteristics of SEP events to advance beyond statistical analysis of single point measurements. Although there have been few large SEP events thus far in cycle 24, there have been a number of smaller events that have been detected by more than one spacecraft. The composition of these SEP events, as indicated by the H/He and Fe/O abundance ratios, shows a dependence on longitudinal distance from the solar source in some events, at times with ratios varying by an order of magnitude. However, these variations are not organized by either the speed or width of the associated coronal mass ejections.",
"doi": "10.1063/1.4723596",
"isbn": "978-0-7354-1026-8",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2012",
"pages": "103-109"
},
{
"id": "authors:38agc-jgp60",
"collection": "authors",
"collection_id": "38agc-jgp60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110118-090120711",
"type": "article",
"title": "Multipoint connectivity analysis of the May 2007 solar energetic particle events",
"author": [
{
"family_name": "Chollet",
"given_name": "E. E.",
"clpid": "Chollet-E-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Gosling",
"given_name": "J. T.",
"clpid": "Gosling-J-T"
},
{
"family_name": "Haggerty",
"given_name": "D. K.",
"orcid": "0000-0001-6395-8943",
"clpid": "Haggerty-D-K"
},
{
"family_name": "Hu",
"given_name": "Q.",
"clpid": "Hu-Q"
},
{
"family_name": "Larson",
"given_name": "D.",
"clpid": "Larson-D"
},
{
"family_name": "Lavraud",
"given_name": "B.",
"clpid": "Lavraud-B"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Opitz",
"given_name": "A.",
"clpid": "Opitz-A"
},
{
"family_name": "Roelof",
"given_name": "E. C.",
"orcid": "0000-0002-2270-0652",
"clpid": "Roelof-E-C"
},
{
"family_name": "Russell",
"given_name": "C. T.",
"orcid": "0000-0003-1639-8298",
"clpid": "Russell-C-T"
},
{
"family_name": "Sauvaud",
"given_name": "J.\u2010A.",
"clpid": "Sauvaud-J-A"
}
],
"abstract": "In May of 2007, the STEREO Ahead and Behind spacecraft, along with the ACE spacecraft situated between the two STEREO spacecraft, observed two small solar energetic particle (SEP) events. STEREO-A and -B observed nearly identical time profiles in the 19 May event, but in the 23 May event, the protons arrived significantly earlier at STEREO-A than at STEREO-B and the time-intensity profiles were markedly different. We present SEP anisotropy, suprathermal electron pitch angle and solar wind data to demonstrate distortion in the magnetic field topology produced by the passage of multiple interplanetary coronal mass ejections on 22 and 23 May, causing the two spacecraft to magnetically connect to different points back at the Sun. This pair of events illustrates the power of multipoint observations in detailed interpretation of complex events, since only a small shift in observer location results in different magnetic field line connections and different SEP time-intensity profiles.",
"doi": "10.1029/2010JA015552",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2010-12-11",
"volume": "115",
"pages": "Art. No. A12106"
},
{
"id": "authors:d0mwj-88n55",
"collection": "authors",
"collection_id": "d0mwj-88n55",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101209-103120218",
"type": "article",
"title": "Record-setting Cosmic-ray Intensities in 2009 and 2010",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "We report measurements of record-setting intensities of cosmic-ray nuclei from C to Fe, made with the Cosmic Ray Isotope Spectrometer carried on the Advanced Composition Explorer in orbit about the inner Sun-Earth Lagrangian point. In the energy interval from ~70 to ~450 MeV nucleon^(\u20131), near the peak in the near-Earth cosmic-ray spectrum, the measured intensities of major species from C to Fe were each 20%-26% greater in late 2009 than in the 1997-1998 minimum and previous solar minima of the space age (1957-1997). The elevated intensities reported here and also at neutron monitor energies were undoubtedly due to several unusual aspects of the solar cycle 23/24 minimum, including record-low interplanetary magnetic field (IMF) intensities, an extended period of reduced IMF turbulence, reduced solar-wind dynamic pressure, and extremely low solar activity during an extended solar minimum. The estimated parallel diffusion coefficient for cosmic-ray transport based on measured solar-wind properties was 44% greater in 2009 than in the 1997-1998 solar-minimum period. In addition, the weaker IMF should result in higher cosmic-ray drift velocities. Cosmic-ray intensity variations at 1 AU are found to lag IMF variations by 2-3 solar rotations, indicating that significant solar modulation occurs inside ~20 AU, consistent with earlier galactic cosmic-ray radial-gradient measurements. In 2010, the intensities suddenly decreased to 1997 levels following increases in solar activity and in the inclination of the heliospheric current sheet. We describe the conditions that gave cosmic rays greater access to the inner solar system and discuss some of their implications.",
"doi": "10.1088/2041-8205/723/1/L1",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2010-11-01",
"series_number": "1",
"volume": "723",
"issue": "1",
"pages": "L1-L6"
},
{
"id": "authors:xsk2t-3gj23",
"collection": "authors",
"collection_id": "xsk2t-3gj23",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100830-135106755",
"type": "article",
"title": "Heavy-ion Fractionation in the Impulsive Solar Energetic Particle Event of 2002 August 20: Elements, Isotopes, and Inferred Charge States",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Measurements of heavy-ion elemental and isotopic composition in the energy range ~12-60 MeV nucleon^(\u20131) are reported from the Advanced Composition Explorer/Solar Isotope Spectrometer (ACE/SIS) instrument for the solar energetic particle (SEP) event of 2002 August 20. We investigate fractionation in this particularly intense impulsive event by examining the enhancements of elemental and isotopic abundance ratios relative to corresponding values in the solar wind. The elemental enhancement pattern is similar to those in other impulsive events detected by ACE/SIS and in compilations of average impulsive-event composition. For individual elements, the abundance of a heavy isotope (mass M_2) is enhanced relative to that of a lighter isotope (M_1) by a factor ~(M_(1)/M_2)^\u03b1 with \u03b1 \u2243 15. Previous studies have reported elemental abundance enhancements organized as a power law in Q/M, the ratio of estimated ionic charge to mass in the material being fractionated. We consider the possibility that a fractionation law of this form could be responsible for the isotopic fractionation as a power law in the mass ratio and then explore the implications it would have for the ionic charge states in the source material. Assuming that carbon is fully stripped (Q_C = 6), we infer mean values of the ionic charge during the fractionation process, Q_Z , for a variety of elements with atomic numbers 7 \u2264 Z \u2264 28. We find that Q_(Fe) \u2243 21-22, comparable to the highest observed values that have been reported at lower energies in impulsive SEP events from direct measurements near 1 AU. The inferred charge states as a function of Z are characterized by several step increases in the number of attached electrons, Z \u2013 Q_Z . We discuss how this step structure, together with the known masses of the elements, might account for a variety of features in the observed pattern of elemental abundance enhancements. We also briefly consider alternative fractionation laws and the relationship between the charge states we infer in the source material and those derived from in situ observations.",
"doi": "10.1088/0004-637X/719/2/1212",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2010-08-20",
"series_number": "2",
"volume": "719",
"issue": "2",
"pages": "1212-1229"
},
{
"id": "authors:yafg6-vhh84",
"collection": "authors",
"collection_id": "yafg6-vhh84",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100921-082613682",
"type": "book_section",
"title": "STEREO and ACE Observations of Energetic Particles from Corotating Interaction Regions",
"book_title": "Twelfth International Solar Wind Conference",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Maksimovic",
"given_name": "Milan",
"clpid": "Maksimovic-M"
}
],
"abstract": "Since early 2007, significant particle enhancements due to corotating interaction regions (CIRs) have regularly appeared at 1 AU without any appreciable contamination from solar energetic particles (SEPs). In 2009 the prevalence of CIRs diminished as the maximum speed of the high speed solar wind streams in the ecliptic decreased along with the tilt of the heliospheric current sheet. Observations of CIR time profiles at different longitudes from STEREO show delays between the Behind and Ahead spacecraft that are often roughly as expected from the corotation time lag, although small differences in the spacecraft latitudes introduce significant scatter in the time delays. In some cases different features seen at Ahead and Behind suggest that transient disturbances in the solar wind may alter connection to or transport from the shock, or that temporal changes occur in the CIR shock itself. H and He data from STEREO/LET at 1.8\u20136 MeV/nucleon show that 1) the CIR spectral index at these energies is ~\u22124, independent of intensity but with considerable variability, 2) the He/H ratio is ~0.03 for larger CIRs but varies systematically with energy and event intensity, and 3) although the correlation between the CIR MeV particle increases and solar wind speed is generally good, many times a high-speed stream is not associated with MeV particles, while at other times a recurring series of CIR particle increases appears only at higher energies and may be associated with current sheet crossings and low speed solar wind.",
"doi": "10.1063/1.3395881",
"isbn": "978-0-7354-0759-6",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2010-03-25",
"pages": "379-382"
},
{
"id": "authors:x3gcd-z8n46",
"collection": "authors",
"collection_id": "x3gcd-z8n46",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100921-085601924",
"type": "book_section",
"title": "Observations and Interpretations of Energetic Neutral Hydrogen Atoms from the December 5, 2006 Solar Event",
"book_title": "Twelfth International Solar Wind Conference",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Shih",
"given_name": "A. Y.",
"clpid": "Shih-A-Y"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Barghouty",
"given_name": "A. F.",
"clpid": "Barghouty-A-F"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Maksimovic",
"given_name": "Milan",
"clpid": "Maksimovic-M"
}
],
"abstract": "We discuss recently reported observations of energetic neutral hydrogen atoms (ENAs) from an X9 solar flare/coronal mass ejection event on 5 December 2006, located at E79. The observations were made by the Low Energy Telescopes (LETs) on STEREO A and B. Prior to the arrival of the main solar energetic particle (SEP) event at Earth, both LETs observed a sudden burst of 1.6 to 15 MeV energetic neutral hydrogen atoms produced by either flare or shock-accelerated protons. RHESSI measurements of the 2.2-MeV \u03b3-ray line provide an estimate of the number of interacting flare-accelerated protons in this event, which leads to an improved estimate of ENA production by flare-accelerated protons. Taking into account ENA losses, we find that the observed ENAs must have been produced in the high corona at heliocentric distances \u2265 2 solar radii. Although there are no CME images from this event, it is shown that CME-shock-accelerated protons can, in principle, produce a time-history consistent with the observations.",
"doi": "10.1063/1.3395935",
"isbn": "978-0-7354-0759-6",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2010-03-25",
"pages": "592-595"
},
{
"id": "authors:p7dk5-8vx42",
"collection": "authors",
"collection_id": "p7dk5-8vx42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160420-081255610",
"type": "book_section",
"title": "Observations of a ^3He-rich SEP Event over a Broad Range of Heliographic Longitudes: Results from STEREO and ACE",
"book_title": "12th International Solar Wind Conference",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "G\u00f3mez-Herrero",
"given_name": "R.",
"clpid": "G\u00f3mez-Herrero-R"
},
{
"family_name": "Haggerty",
"given_name": "D.",
"clpid": "Haggerty-D"
},
{
"family_name": "Nitta",
"given_name": "N. V.",
"clpid": "Nitta-N-V"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Chollet",
"given_name": "E. E.",
"clpid": "Chollet-E-E"
},
{
"family_name": "Cummings",
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"abstract": "Observations of energetic ions and electrons from STEREO and ACE have been used to investigate the longitudinal extent of particle emissions from 3He \u2010rich solar energetic particle (SEP) events. In the event of 3\u20134 Nov 2008, ions and electrons were detected 20\u00b0 ahead and behind the nominal connection from the source region to 1 AU, and electrons were also detected 60\u00b0 ahead. The results are consistent with those of earlier studies that correlated data from near\u2010Earth spacecraft with Helios data or with observations of source regions on the Sun.",
"doi": "10.1063/1.3395943",
"isbn": "978-0-7354-0759-6",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2010-03-25",
"pages": "621-624"
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"title": "First LIGO search for gravitational wave bursts from cosmic (super)strings",
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{
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"given_name": "Alan J.",
"orcid": "0000-0002-0928-6784",
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{
"literal": "LIGO Scientific Collaboration"
}
],
"abstract": "We report on a matched-filter search for gravitational wave bursts from cosmic string cusps using LIGO data from the fourth science run (S4) which took place in February and March 2005. No gravitational waves were detected in 14.9 days of data from times when all three LIGO detectors were operating. We interpret the result in terms of a frequentist upper limit on the rate of gravitational wave bursts and use the limits on the rate to constrain the parameter space (string tension, reconnection probability, and loop sizes) of cosmic string models. Many grand unified theory-scale models (with string tension G\u00b5/c^2[approximate]10^(-6)) can be ruled out at 90% confidence for reconnection probabilities p<=10^(-3) if loop sizes are set by gravitational back reaction.",
"doi": "10.1103/PhysRevD.80.062002",
"issn": "2470-0010",
"publisher": "American Physical Society",
"publication": "Physical Review D",
"publication_date": "2009-09-23",
"series_number": "6",
"volume": "80",
"issue": "6",
"pages": "Art. No. 062002"
},
{
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"collection_id": "e986n-xa711",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091013-093452473",
"type": "article",
"title": "Radial and latitudinal gradients of anomalous cosmic ray oxygen in the inner heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Tranquille",
"given_name": "C.",
"clpid": "Tranquille-C"
},
{
"family_name": "Marsden",
"given_name": "R. G.",
"clpid": "Marsden-R-G"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "We use data from the Ulysses, Advanced Composition Explorer, and Solar Terrestrial Relations Observatory spacecraft to determine the radial and latitudinal gradients of anomalous cosmic ray oxygen in two energy ranges from 4.5\u201315.6 MeV/nuc in the inner heliosphere for the first time during an A<0 part of the solar cycle. Using measurements from early 2007 to mid-2008, we find that the radial gradient is \u223c48 \u00b1 13%/AU, consistent with previous inferences for A<0 and larger than that determined in the inner heliosphere for A>0. The latitudinal gradient is consistent with zero and in the range \u22120.3 to 0.4%/degree, suggesting that during A<0 these particles are not able to propagate into the inner heliosphere by rapid drift along the heliospheric current sheet if the tilt of the sheet is as large as 30 degrees.",
"doi": "10.1029/2009GL039851",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "2009-09-19",
"series_number": "18",
"volume": "36",
"issue": "18",
"pages": "L18103"
},
{
"id": "authors:z18q5-6p558",
"collection": "authors",
"collection_id": "z18q5-6p558",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090817-144816744",
"type": "article",
"title": "Transient intensity changes of cosmic rays beyond the heliospheric termination shock as observed at Voyager 1",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"abstract": "This paper continues our studies of temporal variations of cosmic rays beyond the heliospheric termination shock (HTS) using Voyager 1 (V1) data when V1 was beyond 94 AU. This new study utilizes cosmic ray protons and electrons of several energies. Notable transient decreases of 5\u201350% are observed in galactic cosmic ray nuclei and electrons at V1 shortly after similar decreases are observed at Voyager 2 (V2) still inside the HTS. These decreases at V1 appear to be related to the large solar events in September 2005 and December 2006 and the resulting outward moving interplanetary shock. These two large interplanetary shocks were the largest observed at V2 after V1 crossed the HTS at the end of 2004. They were observed at V2 just inside the HTS at 2006.16 and 2007.43 providing timing markers for V1. From the timing of the intensity decreases observed at V1 as the shocks first reach the HTS and then later reach V1 itself, we can estimate the shock speed beyond the HTS to be between 240 and 300 km s^(\u22121) in both cases. From the timing of the decreases observed when the shock first reaches the HTS and then several months later encounters the heliopause, we can estimate the heliosheath thickness to be 31 \u00b1 4 and 37 \u00b1 6 AU, respectively, for the two sequences of three decreases seen at V1. These values, along with the distances to the HTS that are determined, give distances from the Sun to the heliopause of 121 \u00b1 4 and 124 \u00b1 6 AU, respectively.",
"doi": "10.1029/2009JA014156",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2009-07-30",
"series_number": "7",
"volume": "114",
"issue": "7",
"pages": "A07108"
},
{
"id": "authors:fef0s-40h45",
"collection": "authors",
"collection_id": "fef0s-40h45",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091009-094741170",
"type": "article",
"title": "Elemental Composition and Energy Spectra of Galactic Cosmic Rays During Solar Cycle 23",
"author": [
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"abstract": "We report improved measurements of elemental abundances and spectra for galactic cosmic-ray (GCR) nuclei obtained by the Cosmic Ray Isotope Spectrometer on board NASA's Advanced Composition Explorer (ACE) spacecraft during the minimum and maximum phases of solar cycle 23. We discuss results for particles with nuclear charge 5 \u2264 Z \u2264 28 and typical energies between 50 and 500 MeV nucleon^(\u20131). We demonstrate that a detailed \"leaky box\" Galactic propagation model combined with a spherically symmetric solar modulation model gives a good (but not perfect) fit to the observed spectra by using a solar modulation parameter of \u03c6 = 325 MV at solar minimum and \u03c6 = 900 MV at solar maximum. Although our results are generally consistent with previous measurements from space-based and balloon-based missions, there are significant differences. The large geometrical acceptance and excellent charge resolution of the instrument result in the most detailed and statistically significant record of GCR composition to date in this energy range. The measurements reported here serve as a high-precision baseline for continued studies of GCR composition, solar modulation over the solar cycle, space radiation hazards, and other applications.",
"doi": "10.1088/0004-637X/698/2/1666",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-06-20",
"series_number": "2",
"volume": "689",
"issue": "2",
"pages": "1666-1681"
},
{
"id": "authors:g4w6c-bz545",
"collection": "authors",
"collection_id": "g4w6c-bz545",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-101854474",
"type": "article",
"title": "The Solar Energetic Particle Event of 14 December 2006",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Richardson",
"given_name": "I. G.",
"orcid": "0000-0002-3855-3634",
"clpid": "Richardson-I-G"
},
{
"family_name": "Reames",
"given_name": "D. V.",
"clpid": "Reames-D-V"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "The solar energetic particle event on 14 December 2006 was observed by several near-Earth spacecraft including the Advanced Composition Explorer (ACE), STEREO A and B, SOHO and Wind. An interesting feature of this event is a series of unusual fluctuations in the particle intensity that occurred during the first few hours. These fluctuations were observed inside a magnetic cloud that originated in a solar event on 13 December and show both similarities and variations at the different spacecraft. Interestingly, the most striking difference is between observations at the two closely-separated STEREO spacecraft. In particular, large fluctuations in the proton intensity were seen by the High Energy Telescope (HET) on STEREO A, and to a lesser extent at Wind and ACE, but not by the STEREO B HET. We conclude that the differences in intensity-time profiles were caused by anisotropies in the particle distribution and the different viewing directions of the individual particle telescopes. The intensity/anisotropy variations suggest that flux tubes with different particle propagation conditions existed within this magnetic cloud despite the absence of local magnetic field signatures associated with these regions. The intensity fluctuations are similar to those occasionally seen in impulsive particle events. There were also spacecraft-to-spacecraft differences during the onset of the particle event. An initial rapid onset of energetic (>\u200940 MeV) protons was observed by the STEREO A and B spacecraft outside the magnetic cloud, but not by spacecraft such as SOHO that were already inside the magnetic cloud at this time. The latter spacecraft observed a slower, lower intensity increase. Evidently, energetic proton propagation from the solar event to the vicinity of Earth was inhibited within the magnetic cloud compared to outside.",
"doi": "10.1007/s11207-009-9353-6",
"issn": "0038-0938",
"publisher": "Springer",
"publication": "Solar Physics",
"publication_date": "2009-05",
"series_number": "1-2",
"volume": "256",
"issue": "1-2",
"pages": "443-462"
},
{
"id": "authors:r1gwt-09x60",
"collection": "authors",
"collection_id": "r1gwt-09x60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090918-091120378",
"type": "article",
"title": "STEREO Observations of Energetic Neutral Hydrogen Atoms During the 2006 December 5 Solar Flare",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Barghouty",
"given_name": "A. F.",
"clpid": "Barghouty-A-F"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "von-Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "We report the discovery of energetic neutral hydrogen atoms (ENAs) emitted during the X9 solar event of 2006 December 5. Beginning ~1 hr following the onset of this E79 flare, the Low Energy Telescopes (LETs) on both the STEREO A and B spacecraft observed a sudden burst of 1.6-15 MeV protons beginning hours before the onset of the main solar energetic particle event at Earth. More than 70% of these particles arrived from a longitude within \u00b110\u00b0 of the Sun, consistent with the measurement resolution. The derived emission profile at the Sun had onset and peak times remarkably similar to the GOES soft X-ray profile and continued for more than an hour. The observed arrival directions and energy spectrum argue strongly that the particle events < 5 MeV were due to ENAs. To our knowledge, this is the first reported observation of ENA emission from a solar flare/coronal mass ejection. Possible origins for the production of ENAs in a large solar event are considered. We conclude that the observed ENAs were most likely produced in the high corona and that charge-transfer reactions between accelerated protons and partially stripped coronal ions are an important source of ENAs in solar events.",
"doi": "10.1088/0004-637X/693/1/L11",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2009-03-01",
"series_number": "1",
"volume": "693",
"issue": "1",
"pages": "L11-L15"
},
{
"id": "authors:fsgcj-kk470",
"collection": "authors",
"collection_id": "fsgcj-kk470",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150522-161152863",
"type": "book_section",
"title": "Multi-Point Observations of Corotating Interaction Regions from STEREO and ACE",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Although solar energetic particle (SEP)\nactivity has been at a minimum for the last few years,\nsignificant particle enhancements due to corotating\ninteraction regions (CIRs) have regularly appeared\nat 1 AU, providing an ideal opportunity to study CIR\nparticles without SEP contamination. Observations\nof CIR time profiles from the two STEREO spacecraft\ncommonly show delays that are often roughly\nas expected from the corotation time lag between\nthe two spacecraft. However, in many cases different\nfeatures seen at Ahead and Behind may suggest\nthat transient disturbances in the solar wind alter\nconnection to or transport from the shock, or that\ntemporal changes occur in the CIR shock itself. We\npresent CIR observations from STEREO and ACE\nat energies from ~2-10 MeV/nucleon and examine\nthe evolution of CIR time profiles as a function\nof spacecraft separation in longitude, radius, and\nheliographic latitude.",
"publisher": "Caltech Library",
"publication_date": "2009"
},
{
"id": "authors:g2nyx-nmc05",
"collection": "authors",
"collection_id": "g2nyx-nmc05",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150506-152948443",
"type": "book_section",
"title": "A Comparison of ACE/CRIS Measurements of Galactic\n Cosmic-Ray Abundances and Energy Spectra for Two\n Successive Solar Minima",
"author": [
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Using current solar minimum measurements\nfrom the Cosmic Ray Isotope Spectrometer\n(CRIS) onboard the Advanced Composition Explorer\n(ACE), we report the observed elemental abundances\nand energy spectra for C, 0, Si, and Fe in the energy\nrange of ~50-500 MeV/nucleon. These measurements\nare compared to prior CRIS observations for the\n1997-98 solar minimum period, when the solar magnetic\nfield was of the opposite polarity. By April 2009,\nthe current solar minimum intensities for each of\nthe four elements has surpassed the peak intensities\nobserved during the previous solar minimum. We\nalso examine the correlation of the galactic cosmicray\nintensities with the tilt angle of the heliospheric\ncurrent sheet. These studies will be important for\nunderstanding solar modulation processes, such as\nchanges in drift effects during a solar cycle.",
"publisher": "High Energy Physics Department, University of Lodz",
"publication_date": "2009"
},
{
"id": "authors:4fc60-68z77",
"collection": "authors",
"collection_id": "4fc60-68z77",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150522-161459034",
"type": "book_section",
"title": "Observation and Interpretation of Energetic Neutral Hydrogen Atoms from the December 5, 2006 Solar Flare",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Shih",
"given_name": "A. Y.",
"clpid": "Shih-Albert-Y"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Barghouty",
"given_name": "A. F.",
"clpid": "Barghouty-A-F"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Although solar energetic particle (SEP)\nactivity has been at a minimum for the last few years,\nsignificant particle enhancements due to corotating\ninteraction regions (CIRs) have regularly appeared\nat 1 AU, providing an ideal opportunity to study CIR\nparticles without SEP contamination. Observations\nof CIR time profiles from the two STEREO spacecraft\ncommonly show delays that are often roughly\nas expected from the corotation time lag between\nthe two spacecraft. However, in many cases different\nfeatures seen at Ahead and Behind may suggest\nthat transient disturbances in the solar wind alter\nconnection to or transport from the shock, or that\ntemporal changes occur in the CIR shock itself. We\npresent CIR observations from STEREO and ACE\nat energies from ~2-10 MeV/nucleon and examine\nthe evolution of CIR time profiles as a function\nof spacecraft separation in longitude, radius, and\nheliographic latitude.",
"publisher": "Caltech Library",
"publication_date": "2009"
},
{
"id": "authors:34djg-thr32",
"collection": "authors",
"collection_id": "34djg-thr32",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150512-093515859",
"type": "book_section",
"title": "Multipoint Observations of ^3He-rich Solar Energetic Particle Events using STEREO and ACE",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "G\u00f3mez-Herrero",
"given_name": "R.",
"clpid": "G\u00f3mez-Herrero-R"
},
{
"family_name": "Haggerty",
"given_name": "D. K.",
"orcid": "0000-0001-6395-8943",
"clpid": "Haggerty-D-K"
},
{
"family_name": "Nitta",
"given_name": "N. V.",
"clpid": "Nitta-N-V"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Chollet",
"given_name": "E. E.",
"clpid": "Chollet-E-E"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "M\u00fcller-Mellin",
"given_name": "R.",
"clpid": "M\u00fcller-Mellin-R"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008",
"clpid": "Desai-M-I"
},
{
"family_name": "Mall",
"given_name": "U.",
"clpid": "Mall-U"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Multipoint observations of He-rich solar energetic particle (SEP) events using instruments on the ACE and STEREO have been made over the period January 2007 to May 2009, during which the separation between the two STEREO spacecraft\nin heliolongitude increased from ~0.5\u00b0 to 95\u00b0. Relatively\nquiet conditions on the Sun allowed identification of probable source regions. In one event (4 November 2008), ions were detected at STEREOB and ACE and electrons at all three spacecraft. The longitudinal distributions of energetic particles from ^3He-rich SEP events are discussed and compared with results from previous studies.",
"publisher": "Caltech Library",
"publication_date": "2009"
},
{
"id": "authors:p21wg-q3b49",
"collection": "authors",
"collection_id": "p21wg-q3b49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150527-091845568",
"type": "book_section",
"title": "The Unusual Behavior of Anomalous and Galactic Cosmic Ray Intensities at 1 AU During the Present Solar Minimum",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Since the early 1970's, anomalous cosmic ray (ACR) intensities at 1 AU at solar minimum have generally tracked the galactic cosmic ray (GCR) intensities as measured by neutron monitors. Throughout the current A<0 cycle, however, the ACR intensities are a factor of 3-4 lower than expected from scaling neutron monitor rates; a similar discrepancy seems to have been present during the last A<0\nperiod in the mid-1980's. Also, although there have\nbeen no major solar particle events for over 2 years,\nand sunspot numbers have been at minimum levels\nfor at least a year, the ACR intensities are at present a\nfactor of ~2 lower than their maximum values during\neach of the last 3 solar minima, suggesting that\nheliospheric conditions are not yet at minimum modulation\nlevels. This is probably associated with the fact that ACRs drift inward along the heliospheric current sheet (HCS) during A<0 cycles, and the tilt of the current sheet is still relatively high (~23\ufffd) for solar minimum. However, while ACR intensities are low, GCR intensities are at a record high, and compared with the last A<0 cycle, we find that both ACR and GCR intensities are actually much higher now for a given HCS tilt angle than they were in the mid-1980's.",
"publisher": "Caltech Library",
"publication_date": "2009"
},
{
"id": "authors:kk936-xtv41",
"collection": "authors",
"collection_id": "kk936-xtv41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150512-094808562",
"type": "book_section",
"title": "Time Dependent Composition in the December 2006 SEP Events",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Chollet",
"given_name": "E. E.",
"clpid": "Chollet-E-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008",
"clpid": "Desai-M-I"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Multipoint observations of He-rich solar energetic particle (SEP) events using instruments on the ACE and STEREO have been made over the period January 2007 to May 2009, during which the separation between the two STEREO spacecraft\nin heliolongitude increased from 0.5 to 95 . Relatively\nquiet conditions on the Sun allowed identification of probable source regions. In one event (4 November 2008), ions were detected at STEREOB and ACE and electrons at all three spacecraft. The longitudinal distributions of energetic particles from He-rich SEP events are discussed and compared with results from previous studies.",
"publisher": "Caltech Library",
"publication_date": "2009"
},
{
"id": "authors:9dmrh-vj887",
"collection": "authors",
"collection_id": "9dmrh-vj887",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150528-144715835",
"type": "book_section",
"title": "A Comparison of ACE Measurements of Galactic Cosmic-Ray Abundances and Energy Spectra for Two Successive Solar Minima",
"author": [
{
"family_name": "Lav\u00e9",
"given_name": "J.",
"clpid": "Lav\u00e9-J"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Using current solar minimum measurements from the Cosmic Ray Isotope Spectrometer (CRIS) onboard the Advanced Composition Explorer (ACE), we report the observed elemental abundances and energy spectra for C, O, Si, and Fe in the energy range of ~50-500MeV/nucleon. These measurements are compared to prior CRIS observations for the\n1997-98 solar minimum period, when the solar magnetic\nfield was of the opposite polarity. By April 2009, the current solar minimum intensities for each of the four elements has surpassed the peak intensities observed during the previous solar minimum. We also examine the correlation of the galactic cosmic ray intensities with the tilt angle of the heliospheric current sheet. These studies will be important for understanding solar modulation processes, such as changes in drift effects during a solar cycle.",
"publisher": "Caltech Library",
"publication_date": "2009"
},
{
"id": "authors:2dep4-5aa85",
"collection": "authors",
"collection_id": "2dep4-5aa85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150512-092059942",
"type": "book_section",
"title": "Ionic Charge States Inferred from Elemental and Isotopic Composition in ^3He-rich Solar Energetic Particle Events",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Data from the ACE Solar Isotope Spectrometer have been used to study heavy ion elemental and isotopic abundances at energies above 10MeV/nuc in a number of ^3He-rich solar energetic particle events. The isotopic composition observations have revealed a fractionation pattern in which heavy isotopes are enhanced relative to lighter isotopes\nof the same element as a power law in the ratio of the masses. Adopting the assumption that this represents a special case of a general fractionation law in which different ion species are fractionated as a power law in\nQ/M , we infer ionic charge state values (Q) for a number of elements and compare them with direct measurements, when available. The relationship between these Q values and the observed elemental fractionation patterns are discussed.",
"publisher": "Caltech Library",
"publication_date": "2009"
},
{
"id": "authors:v2dns-xsj24",
"collection": "authors",
"collection_id": "v2dns-xsj24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150528-144033949",
"type": "book_section",
"title": "Time Dependence of Solar Modulation throughout Solar Cycle 23 as Inferred from ACE Measurements of Cosmic-Ray Energy Spectra",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Lave",
"given_name": "K. A.",
"clpid": "Lave-K-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Szabelski",
"given_name": "Jacek",
"clpid": "Szabelski-J"
},
{
"family_name": "Giller",
"given_name": "M.",
"clpid": "Giller-M"
}
],
"abstract": "Since the launch of the Advanced Composition Explorer (ACE) in August 1997, the Cosmic Ray Isotope Spectrometer (CRIS) has been providing measurements of cosmic-ray energy spectra between \u223c50 and \u223c500 MeV/nuc for a wide range of elements. The shape of these low-energy spectra, which are\nmeasured with good statistical precision on time scales as short as a solar rotation, are strongly influenced by modulation in the heliosphere. By combining calculated local interstellar spectra from a leaky-box propagation model with a sphericallysymmetric, steady-state model of solar modulation, we have derived the time dependence of the modulation strength throughout solar cycle 23. In addition, we have investigated hysteresis effects in the modulation by comparing time dependences at different\nenergies in two ways. First, we have compared values of the modulation parameter, \u03c6, calculated based on CRIS spectral measurements with published values derived from neutron monitor data. Second, we have studied effects over relatively small energy ranges by comparing CRIS intensity measurements at different energies. We report the ACE/CRIS observations, discuss the trends in the data, and compare with previous results on the variations of the solar modulation level over the solar cycle.",
"publisher": "Caltech Library",
"publication_date": "2009"
},
{
"id": "authors:rzfjy-c5372",
"collection": "authors",
"collection_id": "rzfjy-c5372",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:WEBjgra08",
"type": "article",
"title": "Galactic cosmic ray H and He nuclei energy spectra measured by Voyagers 1 and 2 near the heliospheric termination shock in positive and negative solar magnetic polarity cycles",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"abstract": "Using data from the Voyager 1 and 2 spacecraft, we have followed the intensity variations of H, He and C + O nuclei between 1998 and 2008 and determined the spectra for H and He at the time of minimum modulation in 1998, when the solar magnetic polarity was positive and again in 2008 when the solar magnetic polarity was negative. At these times these data are representative of conditions near a heliospheric termination shock assumed to be located at \u223c90 AU. Above \u223c400 MeV/nuc for He nuclei the 11-year solar modulation cycle observed at the Earth is not seen; instead there is a 22-year variation. The negative polarity cycle intensities above \u223c150 MeV/nuc are higher than those in the positive polarity cycle by a factor of 1.4\u20131.7 times for both H and He nuclei. Below \u223c100 MeV/nuc the C nuclei intensities are similar in the two cycles to within \u00b110%. These observations are compared with theoretical calculations which also show a negative to positive polarity cycle intensity difference at higher energies, most likely associated with energy changes due to drifts near the termination shock, but the comparison suggests that improved estimates of the local interstellar spectra are required.",
"doi": "10.1029/2008JA013395",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2008-10-28",
"series_number": "A10",
"volume": "113",
"issue": "A10",
"pages": "A10108"
},
{
"id": "authors:95gns-pw536",
"collection": "authors",
"collection_id": "95gns-pw536",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BINnar08",
"type": "article",
"title": "The OB association origin of galactic cosmic rays",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Arnould",
"given_name": "M.",
"clpid": "Arnould-M"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Goriely",
"given_name": "S.",
"clpid": "Goriely-S"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The isotopic abundances of neon, iron, and a number of other species in the galactic cosmic rays have been measured using the Cosmic Ray Isotope Spectrometer (CRIS) aboard the NASA Advanced Composition Explorer (ACE) spacecraft. We compare our data to results from two-component Wolf-Rayet (WR) models. The largest deviations of galactic cosmic ray (GCR) isotope ratios from solar-system ratios predicted by these models are ^C12/^O16, ^Ne22/^Ne20, and ^Fe58/^Fe56. Our measured abundance ratios show good agreement with the model predictions. All of our measured isotopic ratios are consistent with a GCR source consisting of ~20% of WR material mixed with ~80% material with solar-system composition. Since WR stars are evolutionary products of OB stars, and most OB stars exist in OB associations, the good agreement of our data with these models strongly suggests that OB associations are the most probable source of at least a substantial fraction of GCRs. In previous work we have shown that the primary ^Ni59 (which is radioactive and decays only by electron-capture) synthesized in supernovae has decayed prior to being accelerated to GCRs, indicating a time interval between nucleosynthesis and acceleration of >10^5 yr. In this paper we describe a scenario that should allow most of the ^Ni59 to decay in the OB association environment and conclude that OB associations are the likely source of most GCRs.",
"doi": "10.1016/j.newar.2008.05.008",
"issn": "1387-6473",
"publisher": "Elsevier",
"publication": "New Astronomy Reviews",
"publication_date": "2008-10",
"series_number": "7-10",
"volume": "52",
"issue": "7-10",
"pages": "427-430"
},
{
"id": "authors:rbjbc-k2290",
"collection": "authors",
"collection_id": "rbjbc-k2290",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090528-101806583",
"type": "book_section",
"title": "Anomalous cosmic rays in the heliosheath",
"book_title": "Particle Acceleration and Transport in the Heliosphere and Beyond",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-Nand"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Li",
"given_name": "Gang",
"clpid": "Li-Gang"
},
{
"family_name": "Hu",
"given_name": "Qiang",
"clpid": "Hu-Qiang"
},
{
"family_name": "Verkhoglyadova",
"given_name": "Olga",
"clpid": "Verkhoglyadova-O"
},
{
"family_name": "Zank",
"given_name": "Gary P.",
"clpid": "Zank-G-P"
},
{
"family_name": "Lin",
"given_name": "R. P.",
"clpid": "Lin-R-P"
},
{
"family_name": "Luhmann",
"given_name": "J.",
"clpid": "Luhmann-J-G"
}
],
"abstract": "We report on Voyager 1 and 2 observations of anomalous cosmic rays in the outer heliosphere. The energy spectrum of anomalous cosmic ray helium as each spacecraft crossed the solar wind termination shock into the heliosheath remained modulated. Assuming the intensity gradient between the two spacecraft is purely radial, we find that radial gradients in the heliosheath of He with 11.6\u201322.3 MeV/nuc and with \u223c61\u201373MeV/nuc\u223c61\u201373\u2009MeV/nuc are 4.9\u00b11.2%/AU4.9\u00b11.2%/AU and 0.0\u00b10.5%/AU,0.0\u00b10.5%/AU, respectively. Strong temporal variations of the 11.6\u201322.3 MeV/nuc He intensity at both spacecraft were observed in 2005 just after Voyager 1 crossed the termination shock and while Voyager 2 was upstream. After 2006.0, the intensity variations are more moderate and likely due to a combination of spatial and temporal variations. As of early 2008, the anomalous cosmic ray He energy spectrum has unfolded to what may be a source spectrum. The spectrum at Voyager 2 remains modulated. We examine three recent models of the origin of anomalous cosmic rays in light of these observations.",
"doi": "10.1063/1.2982469",
"isbn": "9780735405660",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2008-08-25",
"pages": "343-348"
},
{
"id": "authors:bc0b7-2dy22",
"collection": "authors",
"collection_id": "bc0b7-2dy22",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090414-092941101",
"type": "book_section",
"title": "Examination of the last large solar energetic particle events of solar cycle 23",
"book_title": "Particle Acceleration and Transport in the Heliosphere and beyond",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Li",
"given_name": "G.",
"clpid": "Li-Gang"
},
{
"family_name": "Hu",
"given_name": "Q.",
"clpid": "Hu-Q"
},
{
"family_name": "Verkhoglyadova",
"given_name": "O.",
"clpid": "Verkhoglyadova-O"
},
{
"family_name": "Zank",
"given_name": "Gary P.",
"clpid": "Zank-G-P"
},
{
"family_name": "Lin",
"given_name": "R. P.",
"clpid": "Lin-R-P"
},
{
"family_name": "Lulimann",
"given_name": "J.",
"clpid": "Lulimann-J"
}
],
"abstract": "The last two large solar energetic particle (SEP) events of solar cycle 23 were observed in December 2006 by several spacecraft including ACE and STEREO. Active region\nnumber 10930 rotated over the eastern limb of the Sun already generating intense x-ray flares.\nAs it crossed the disk, it produced 4 X-class flares and at least 3 halo coronal mass ejections.\nThe two dominant SEP events occurred when the region was at ~E70 and ~W25. We have\ncombined particle observations from the Solar Isotope Spectrometer (SIS) and the Ultra-Low\nEnergy Isotope Spectrometer (ULEIS) on ACE and the Low Energy Telescope (LET) on\nSTEREO for each event. Energy spectra for many heavy ion species integrated over the\nduration of each SEP event show distinct differences between the two events. We find the\nsecond event (on December 13) has a much harder spectrum above 10 MeV/nucleon and a 12-60\nMeV/nucleon composition substantially enriched in elements with Z>14 as compared to the first\nevent (on December 6). While the December 6 event is similar in Fe/O to other events with\ncomparable fluence in solar cycle 23, the December 13 event has the highest Fe/O ratio of all\nevents with Si fluence > 100 (cm^2 sr MeV/n)^-1. In composition, this second event is most similar\nto the event of November 6, 1997.",
"doi": "10.1063/1.2982432",
"isbn": "9780735405660",
"publisher": "American Institute of Pliysics",
"publication_date": "2008-08-25",
"pages": "118-123"
},
{
"id": "authors:2e2xv-qza75",
"collection": "authors",
"collection_id": "2e2xv-qza75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090507-132736204",
"type": "book_section",
"title": "STEREO and ACE observations of CIR particles",
"book_title": "Particle Acceleration and Transport in the Heliosphere and Beyond\u2014 7th Annual Astrophysics Conference",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Miyasaka",
"given_name": "H.",
"orcid": "0000-0002-8074-4186",
"clpid": "Miyasaka-Hiromasa"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "In the present solar minimum, corotating interaction regions (CIRs) produce frequent particle enhancements at 1 AU as observed at STEREO and ACE. As the two STEREO spacecraft move apart, differences in CIR time profiles observed at each spacecraft are becoming large. The timing differences are often roughly similar to the corotation time lag between the two spacecraft, however many of the features seen at Ahead and Behind require more than just a time shift. Perhaps transient disturbances in the solar wind affect connection to or transport from the shock, or temporal changes occur in the CIR shock itself. Additional timing differences of >1 day result from the different heliographic latitudes of the two STEREO spacecraft",
"doi": "10.1063/1.2982435",
"isbn": "9780735405660",
"publisher": "American Institute of Physics",
"publication_date": "2008-08-25",
"pages": "131-136"
},
{
"id": "authors:xbk8q-17344",
"collection": "authors",
"collection_id": "xbk8q-17344",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090727-132850697",
"type": "book_section",
"title": "Elemental and isotopic fractionation in 3He-rich solar energetic particle events",
"book_title": "Particle Acceleration and Transport in the Heliosphere and Beyond: 7th Annual International Astrophysics Conference",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Li",
"given_name": "G.",
"clpid": "Li-Gang"
},
{
"family_name": "Hu",
"given_name": "Q.",
"clpid": "Hu-Qiang"
},
{
"family_name": "Verkhoglyadova",
"given_name": "G. P.",
"clpid": "Verkhoglyadova-G-P"
},
{
"family_name": "Zank",
"given_name": "Gary P.",
"clpid": "Zank-G-P"
},
{
"family_name": "Lin",
"given_name": "R. P.",
"clpid": "Lin-R-P"
},
{
"family_name": "Lulimann",
"given_name": "J.",
"clpid": "Lulimann-J"
}
],
"abstract": "Using data from the Solar Isotope Spectrometer (SIS) on the Advanced Composition Explorer (ACE) mission, heavy ion composition measurements have been made in 26^3He-rich solar energetic particle (SEP) events that occurred between 1998 and 2004. Relative abundances of 13 elements from C through Ni have been investigated, as have the isotopic compositions of the elements Ne and Mg. We find a general tendency for the abundances to follow trends similar to those found in gradual SEP events, in which fractionation can be represented in the form of a power-law in Q/M. However several deviations from this pattern are noted that may provide useful diagnostics of the acceleration process occurring in solar flares.",
"doi": "10.1063/1.2982438",
"isbn": "9780735405660",
"publisher": "American Institute of Physics",
"place_of_publication": "Kauai, HI",
"publication_date": "2008-08-25",
"pages": "149-155"
},
{
"id": "authors:yeh9t-99d43",
"collection": "authors",
"collection_id": "yeh9t-99d43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-095819459",
"type": "article",
"title": "An asymmetric solar wind termination shock",
"author": [
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "Frank B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "Bryant C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "Nand",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "William R.",
"clpid": "Webber-W-R"
}
],
"abstract": "Voyager 2 crossed the solar wind termination shock at 83.7 au in the southern hemisphere, ~10 au closer to the Sun than found by Voyager 1 in the north. This asymmetry could indicate an asymmetric pressure from an interstellar magnetic field, from transient-induced shock motion, or from the solar wind dynamic pressure. Here we report that the intensity of 4\u20135 MeV protons accelerated by the shock near Voyager 2 was three times that observed concurrently by Voyager 1, indicating differences in the shock at the two locations. (Companion papers report on the plasma, magnetic field, plasma-wave and lower energy particle observations at the shock.) Voyager 2 did not find the source of anomalous cosmic rays at the shock, suggesting that the source is elsewhere on the shock or in the heliosheath. The small intensity gradient of Galactic cosmic ray helium indicates that either the gradient is further out in the heliosheath or the local interstellar Galactic cosmic ray intensity is lower than expected.",
"doi": "10.1038/nature07022",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2008-07-03",
"series_number": "7200",
"volume": "454",
"issue": "7200",
"pages": "71-74"
},
{
"id": "authors:5j7d5-yr416",
"collection": "authors",
"collection_id": "5j7d5-yr416",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:SOLapj08",
"type": "article",
"title": "A novel technique to infer ionic charge states of solar energetic particles",
"author": [
{
"family_name": "Sollitt",
"given_name": "L. S.",
"clpid": "Sollitt-L-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"clpid": "Weidenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "In some large solar energetic particle (SEP) events, the intensities of higher energy SEPs decay more rapidly than at lower energies. This energy dependence varies with particle species, as would be expected if the decay timescale depended on a rigidity-dependent diffusion mean free path. By comparing the decay timescales of carbon, nitrogen, oxygen, neon, magnesium, silicon, sulfur, and iron, mean charge states are inferred for these (and other) elements in three SEP events between 1997 and 2002 at energies between 10 and 200 MeV nucleon\u22121. In a fourth event, upper limits for the charge states are inferred. The charge states of many different particle species are all consistent with a single source temperature; in two events in 1997 and 2002, the best-fit temperature is much higher than that of the corona, which could imply a contribution from solar flare material. However, comparison with lower energy iron charge states for the 1997 event implies that the observed high-energy charge state could also be understood as the result of stripping during shock acceleration in the corona.",
"doi": "10.1086/587121",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2008-05-20",
"series_number": "1",
"volume": "679",
"issue": "1",
"pages": "910-919"
},
{
"id": "authors:0ncnh-kyh91",
"collection": "authors",
"collection_id": "0ncnh-kyh91",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140908-100838268",
"type": "article",
"title": "The Low-Energy Telescope (LET) and SEP Central Electronics for the STEREO Mission",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Geier",
"given_name": "S.",
"orcid": "0000-0002-3948-9339",
"clpid": "Geier-S"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Klemic",
"given_name": "J.",
"clpid": "Klemic-J"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Miyasaka",
"given_name": "H.",
"orcid": "0000-0002-8074-4186",
"clpid": "Miyasaka-Hiromasa"
},
{
"family_name": "Nguyen",
"given_name": "V.",
"clpid": "Nguyen-V"
},
{
"family_name": "Ogliore",
"given_name": "R. C.",
"clpid": "Ogliore-R-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Radocinski",
"given_name": "R. G.",
"clpid": "Radocinski-R-G"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Hawk",
"given_name": "J.",
"clpid": "Hawk-J"
},
{
"family_name": "Shuman",
"given_name": "S.",
"clpid": "Shuman-S"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wortman",
"given_name": "K.",
"clpid": "Wortman-K"
}
],
"abstract": "The Low-Energy Telescope (LET) is one of four sensors that make up the Solar Energetic Particle (SEP) instrument of the IMPACT investigation for NASA's STEREO mission. The LET is designed to measure the elemental composition, energy spectra, angular distributions, and arrival times of H to Ni ions over the energy range from \u223c3 to \u223c30 MeV/nucleon. It will also identify the rare isotope ^(3)He and trans-iron nuclei with 30\u2264Z\u226483. The SEP measurements from the two STEREO spacecraft will be combined with data from ACE and other 1-AU spacecraft to provide multipoint investigations of the energetic particles that result from interplanetary shocks driven by coronal mass ejections (CMEs) and from solar flare events. The multipoint in situ observations of SEPs and solar-wind plasma will complement STEREO images of CMEs in order to investigate their role in space weather. Each LET instrument includes a sensor system made up of an array of 14 solid-state detectors composed of 54 segments that are individually analyzed by custom Pulse Height Analysis System Integrated Circuits (PHASICs). The signals from four PHASIC chips in each LET are used by a Minimal Instruction Set Computer (MISC) to provide onboard particle identification of a dozen species in \u223c12 energy intervals at event rates of \u223c1,000 events/sec. An additional control unit, called SEP Central, gathers data from the four SEP sensors, controls the SEP bias supply, and manages the interfaces to the sensors and the SEP interface to the Instrument Data Processing Unit (IDPU). This article outlines the scientific objectives that LET will address, describes the design and operation of LET and the SEP Central electronics, and discusses the data products that will result.",
"doi": "10.1007/s11214-007-9288-x",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2008-04",
"series_number": "1-4",
"volume": "136",
"issue": "1-4",
"pages": "285-362"
},
{
"id": "authors:jxjvj-d4w12",
"collection": "authors",
"collection_id": "jxjvj-d4w12",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160630-091011138",
"type": "article",
"title": "The High Energy Telescope for STEREO",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Reames",
"given_name": "D. V.",
"clpid": "Reames-D-V"
},
{
"family_name": "Baker",
"given_name": "R.",
"clpid": "Baker-R"
},
{
"family_name": "Hawk",
"given_name": "J.",
"clpid": "Hawk-J"
},
{
"family_name": "Nolan",
"given_name": "J.T.",
"clpid": "Nolan-J-T"
},
{
"family_name": "Ryan",
"given_name": "L.",
"clpid": "Ryan-L"
},
{
"family_name": "Shuman",
"given_name": "S.",
"clpid": "Shuman-S"
},
{
"family_name": "Wortman",
"given_name": "K.A.",
"clpid": "Wortman-K-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "The IMPACT investigation for the STEREO Mission includes a complement of Solar Energetic Particle instruments on each of the two STEREO spacecraft. Of these instruments, the High Energy Telescopes (HETs) provide the highest energy measurements. This paper describes the HETs in detail, including the scientific objectives, the sensors, the overall mechanical and electrical design, and the on-board software. The HETs are designed to measure the abundances and energy spectra of electrons, protons, He, and heavier nuclei up to Fe in interplanetary space. For protons and He that stop in the HET, the kinetic energy range corresponds to \u223c13 to 40 MeV/n. Protons that do not stop in the telescope (referred to as penetrating protons) are measured up to \u223c100 MeV/n, as are penetrating He. For stopping He, the individual isotopes 3He and 4He can be distinguished. Stopping electrons are measured in the energy range \u223c0.7\u20136 MeV.",
"doi": "10.1007/978-0-387-09649-0_14",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2008-04",
"series_number": "1-4",
"volume": "136",
"issue": "1-4",
"pages": "391-435"
},
{
"id": "authors:78tsr-fce19",
"collection": "authors",
"collection_id": "78tsr-fce19",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140908-100947326",
"type": "article",
"title": "STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview",
"author": [
{
"family_name": "Luhmann",
"given_name": "J. G.",
"orcid": "0000-0003-0626-9353",
"clpid": "Luhmann-J-G"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
}
],
"abstract": "The IMPACT (In situ Measurements of Particles And CME Transients) investigation on the STEREO mission was designed and developed to provide multipoint solar wind and suprathermal electron, interplanetary magnetic field, and solar energetic particle information required to unravel the nature of coronal mass ejections and their heliospheric consequences. IMPACT consists of seven individual sensors which are packaged into a boom suite, and a SEP suite. This review summarizes the science objectives of IMPACT, the instruments that comprise the IMPACT investigation, the accommodation of IMPACT on the STEREO twin spacecraft, and the overall data products that will flow from the IMPACT measurements. Accompanying papers in this volume of Space Science Reviews highlight the individual sensor technical details and capabilities, STEREO project plans for the use of IMPACT data, and modeling activities for IMPACT (and other STEREO) data interpretation.",
"doi": "10.1007/s11214-007-9170-x",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2008-04",
"series_number": "1-4",
"volume": "136",
"issue": "1-4",
"pages": "117-184"
},
{
"id": "authors:4fb8v-2vh68",
"collection": "authors",
"collection_id": "4fb8v-2vh68",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140908-091625580",
"type": "article",
"title": "Passage of a large interplanetary shock from the inner heliosphere to the heliospheric termination shock and beyond: Its effects on cosmic rays at Voyagers 1 and 2",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"abstract": "Using data from the charged particle telescopes on V1 and V2 we have followed the progress of a large interplanetary shock as it passes V2 at a distance of 79 AU at about 2006.16, then later crosses the heliospheric termination shock finally reaching V1 at a distance \u223c100 AU. A decrease \u223c15% is observed in the V2 >70 MeV rate starting at 2006.19 and three smaller decreases starting at 2006.29, 2006.50 and 2006.86 are observed at V1. From the timing of the first two decreases at V1 we are able to determine that the average shock speed slows down at the termination shock from \u223c600 km s^(\u22121) to 210\u2013270 km s^(\u22121). Decreases of \u223c30\u201350% in anomalous He and galactic H are observed at V2 when the shock passes this location inside the termination shock. Smaller decreases are observed for both of these components when the weakened interplanetary shock passes V1 at 2006.50. These results define the extent and magnitude of solar modulation effects on cosmic rays caused by transients both inside and beyond the termination shock.",
"doi": "10.1029/2007GL031339",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "2007-10",
"series_number": "20",
"volume": "34",
"issue": "20",
"pages": "Art. No. L20107"
},
{
"id": "authors:czhfs-nkf29",
"collection": "authors",
"collection_id": "czhfs-nkf29",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140905-154130174",
"type": "article",
"title": "Temporal and spectral variations of anomalous oxygen nuclei measured by Voyager 1 and Voyager 2 in the outer heliosphere",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"abstract": "We have studied the temporal and spectral variations of anomalous oxygen nuclei at the Voyager 1 (V1) and 2 (V2) spacecraft in the outer heliosphere from 1990 to the present time in 2006 when V1 is now beyond the heliospheric termination shock. During this time period, the intensities increased from their lowest values in 1990\u20131991 up to a maximum in 1998\u20131999 and then decreased rapidly in 2000\u20132001 in time coincidence with the change in solar magnetic polarity from positive to negative. During the time period after 2001, significant changes in intensities and spectra are observed relative to the earlier period of positive solar magnetic polarity before 2001. It is found that the intensities of O above \u223c10 MeV/nuc at V1 after \u223c2002.0 were higher relative to the same galactic cosmic ray He intensity between 150\u2013380 MeV/nuc than in the earlier time period. As a result, by 2006 these intensities were a factor \u223c3 times those measured at the intensity maximum in 1998\u20131999 in the previous polarity cycle. The changes observed at V2 followed a similar pattern, but the relative intensity changes of O were a factor \u223c2 times greater than those observed at V1. Also, above \u223c10 MeV/nuc, the intensity changes at V1 and V2 were nearly energy independent, and the spectra at all times before and after the solar magnetic polarity change and at all modulation levels remained \u223cE^(\u22123.0\u00b10.2), possibly characteristic of a \"source\" spectrum. When V1 crossed the termination shock, no noticeable spectral or intensity changes were observed.",
"doi": "10.1029/2006JA012207",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2007-06-05",
"series_number": "A6",
"volume": "112",
"issue": "A6",
"pages": "Art. No. A06105"
},
{
"id": "authors:qh4jk-q7h10",
"collection": "authors",
"collection_id": "qh4jk-q7h10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100503-100012820",
"type": "article",
"title": "Solar Elemental Composition Based on Studies of Solar Energetic Particles",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
}
],
"abstract": "Solar abundances can be derived from the composition of the solar wind and solar energetic particles (SEPs) as well as obtained through spectroscopic means. Past comparisons have suggested that all three samples agree well, when rigidity-related fractionation effects on the SEPs were accounted for. It has been known that such effects vary from one event to the next and should be addressed on an event-by-event basis. This paper examines event variability more closely, particularly in terms of energy-dependent SEP abundances. This is now possible using detailed SEP measurements spanning several decades in energy from the Ultra Low Energy Isotope Spectrometer (ULEIS) and the Solar Isotope Spectrometer (SIS) on the ACE spacecraft. We present examples of the variability of the elemental composition with energy and suggest they can be understood in terms of diffusion from the acceleration region near the interplanetary shock. By means of a spectral scaling procedure, we obtain energy-independent abundance ratios for 14 large SEP events and compare them to reported solar wind and coronal abundances as well as to previous surveys of SEP events.",
"doi": "10.1007/s11214-007-9218-y",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2007-06",
"series_number": "1-4",
"volume": "130",
"issue": "1-4",
"pages": "183-194"
},
{
"id": "authors:03nm5-91j72",
"collection": "authors",
"collection_id": "03nm5-91j72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100909-133903373",
"type": "article",
"title": "An Overview of the Origin of Galactic Cosmic Rays as Inferred from Observations of Heavy Ion Composition and Spectra",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The galactic cosmic rays arriving near Earth, which include both stable and long-lived nuclides from throughout the periodic table, consist of a mix of stellar nucleosynthesis products accelerated by shocks in the interstellar medium (ISM) and fragmentation products made by high-energy collisions during propagation through the ISM. Through the study of the composition and spectra of a variety of elements and isotopes in this diverse sample, models have been developed for the origin, acceleration, and transport of galactic cosmic rays. We present an overview of the current understanding of these topics emphasizing the insights that have been gained through investigations in the charge and energy ranges Z \u2272 30 and E/M \u2272 1 GeV/nuc, and particularly those using data obtained from the Cosmic Ray Isotope Spectrometer on NASA's Advanced Composition Explorer mission.",
"doi": "10.1007/s11214-007-9198-y",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2007-06",
"series_number": "1-4",
"volume": "130",
"issue": "1-4",
"pages": "415-429"
},
{
"id": "authors:emp5w-xgp42",
"collection": "authors",
"collection_id": "emp5w-xgp42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100506-100356849",
"type": "article",
"title": "On the Differences in Composition between Solar Energetic Particles and Solar Wind",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008",
"clpid": "Desai-M-I"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Raines",
"given_name": "J.",
"clpid": "Raines-J"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
}
],
"abstract": "Although the average composition of solar energetic particles (SEPs) and the bulk solar wind are similar in a number of ways, there are key differences which imply that solar wind is not the principal seed population for SEPs accelerated by coronal mass ejection (CME) driven shocks. This paper reviews these composition differences and considers the composition of other possible seed populations, including coronal material, impulsive flare material, and interplanetary CME material.",
"doi": "10.1007/s11214-007-9187-1",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2007-06",
"series_number": "1-4",
"volume": "130",
"issue": "1-4",
"pages": "207-219"
},
{
"id": "authors:6chxg-mj695",
"collection": "authors",
"collection_id": "6chxg-mj695",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100503-155507464",
"type": "article",
"title": "An Update on Ultra-Heavy Elements in Solar Energetic Particles above 10 MeV/Nucleon",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Measurements below several MeV/nucleon from Wind/LEMT and ACE/ULEIS show that elements heavier than Zn (Z=30) can be enhanced by factors of ~100 to 1000, depending on species, in ^3He-rich solar energetic particle (SEP) events. Using the Solar Isotope Spectrometer (SIS) on ACE we find that even large SEP (LSEP) shock-accelerated events at energies from ~10 to >100 MeV/nucleon are often very iron rich and might contain admixtures of flare seed material. Studies of ultra-heavy (UH) SEPs (with Z>30) above 10 MeV/nucleon can be used to test models of acceleration and abundance enhancements in both LSEP and ^3He-rich events. We find that the long-term average composition for elements from Z=30 to 40 is similar to standard solar system values, but there is considerable event-to-event variability. Although most of the UH fluence arrives during LSEP events, UH abundances are relatively more enhanced in ^3He-rich events, with the (3410 MeV/nucleon, the most extreme event in terms of UH composition detected so far took place on 23 July 2004 and had a (34",
"doi": "10.1007/s11214-007-9191-5",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2007-06",
"series_number": "1-4",
"volume": "130",
"issue": "1-4",
"pages": "335-340"
},
{
"id": "authors:rbjct-m9t19",
"collection": "authors",
"collection_id": "rbjct-m9t19",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-105038224",
"type": "article",
"title": "OB Associations, Wolf-Rayet Stars, and the Origin of Galactic Cosmic Rays",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Arnould",
"given_name": "M.",
"clpid": "Arnould-M"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Goriely",
"given_name": "S.",
"clpid": "Goriely-S"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Meynet",
"given_name": "G.",
"clpid": "Meynet-G"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "We have measured the isotopic abundances of neon and a number of other species in the galactic cosmic rays (GCRs) using the Cosmic Ray Isotope Spectrometer (CRIS) aboard the ACE spacecraft. Our data are compared to recent results from two-component (Wolf\u2013Rayet material plus solar-like mixtures) Wolf\u2013Rayet (WR) models. The three largest deviations of galactic cosmic ray isotope ratios from solar-system ratios predicted by these models, ^(12)C/^(16)O, ^(22)Ne/^(20)Ne, and ^(58)Fe/^(56)Fe, are very close to those observed. All of the isotopic ratios that we have measured are consistent with a GCR source consisting of \u223c20% of WR material mixed with \u223c80% material with solar-system composition. Since WR stars are evolutionary products of OB stars, and most OB stars exist in OB associations that form superbubbles, the good agreement of our data with WR models suggests that OB associations within superbubbles are the likely source of at least a substantial fraction of GCRs. In previous work it has been shown that the primary ^(59)Ni (which decays only by electron-capture) in GCRs has decayed, indicating a time interval between nucleosynthesis and acceleration of >10^5 y. It has been suggested that in the OB association environment, ejecta from supernovae might be accelerated by the high velocity WR winds on a time scale that is short compared to the half-life of ^(59)Ni. Thus the ^(59)Ni might not have time to decay and this would cast doubt upon the OB association origin of cosmic rays. In this paper we suggest a scenario that should allow much of the ^(59)Ni to decay in the OB association environment and conclude that the hypothesis of the OB association origin of cosmic rays appears to be viable.",
"doi": "10.1007/s11214-007-9195-1",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2007-06",
"series_number": "1-4",
"volume": "130",
"issue": "1-4",
"pages": "439-449"
},
{
"id": "authors:gmcfb-bbh33",
"collection": "authors",
"collection_id": "gmcfb-bbh33",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100503-093124629",
"type": "article",
"title": "Solar Isotopic Composition as Determined Using Solar Energetic Particles",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Solar energetic particles (SEPs) provide a sample of the Sun from which solar composition may be determined. Using high-resolution measurements from the Solar Isotope Spectrometer (SIS) onboard NASA's Advanced Composition Explorer (ACE) spacecraft, we have studied the isotopic composition of SEPs at energies \u226520 MeV/nucleon in large SEP events. We present SEP isotope measurements of C, O, Ne, Mg, Si, S, Ar, Ca, Fe, and Ni made in 49 large events from late 1997 to the present. The isotopic composition is highly variable from one SEP event to another due to variations in seed particle composition or due to mass fractionation that occurs during the acceleration and/or transport of these particles. We show that various isotopic and elemental enhancements are correlated with each other, discuss the empirical corrections used to account for the compositional variability, and obtain estimated solar isotopic abundances. We compare the solar values and their uncertainties inferred from SEPs with solar wind and other solar system abundances and find generally good agreement.",
"doi": "10.1007/s11214-007-9185-3",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2007-06",
"series_number": "1-4",
"volume": "130",
"issue": "1-4",
"pages": "195-205"
},
{
"id": "authors:4nh5v-gxz69",
"collection": "authors",
"collection_id": "4nh5v-gxz69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140716-161335184",
"type": "article",
"title": "Composition of Anomalous Cosmic Rays",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "The \"classic\" anomalous cosmic ray (ACR) component originates as interstellar neutral atoms that drift into the heliosphere, become ionized and picked up by the solar wind, and carried to the outer heliosphere where the pickup ions are accelerated to hundreds of MeV, presumably at the solar wind termination shock. These interstellar ACRs are predominantly singly charged, although higher charge states are present and become dominant above \u223c350 MeV. Their isotopic composition is like that of the solar system and unlike that of the source of galactic cosmic rays. A comparison of their energy spectra with the estimated flux of pickup ions flowing into the termination shock reveals a mass-dependent acceleration efficiency that favors heavier ions. There is also a heliospheric ACR component as evidenced by \"minor\" ACR ions, such as Na, Mg, S, and Si that appear to be singly-ionized ions from a source likely in the outer heliosphere.",
"doi": "10.1007/s11214-007-9161-y",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2007-06",
"series_number": "1-4",
"volume": "130",
"issue": "1-4",
"pages": "389-399"
},
{
"id": "authors:qhk80-8a962",
"collection": "authors",
"collection_id": "qhk80-8a962",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190909-133030848",
"type": "book_section",
"title": "Solar Isotopic Composition as Determined Using Solar Energetic Particles",
"book_title": "The Composition of Matter",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "von Steiger",
"given_name": "Rudolf",
"clpid": "von-Steiger-R"
},
{
"family_name": "Gloeckler",
"given_name": "George",
"clpid": "Gloeckler-G"
},
{
"family_name": "Mason",
"given_name": "Glenn M.",
"clpid": "Mason-G-M"
}
],
"abstract": "Solar energetic particles (SEPs) provide a sample of the Sun from which solar composition may be determined. Using high-resolution measurements from the Solar Isotope Spectrometer (SIS) onboard NASA's Advanced Composition Explorer (ACE) spacecraft, we have studied the isotopic composition of SEPs at energies \u226520 MeV/nucleon in large SEP events. We present SEP isotope measurements of C, O, Ne, Mg, Si, S, Ar, Ca, Fe, and Ni made in 49 large events from late 1997 to the present. The isotopic composition is highly variable from one SEP event to another due to variations in seed particle composition or due to mass fractionation that occurs during the acceleration and/or transport of these particles. We show that various isotopic and elemental enhancements are correlated with each other, discuss the empirical corrections used to account for the compositional variability, and obtain estimated solar isotopic abundances. We compare the solar values and their uncertainties inferred from SEPs with solar wind and other solar system abundances and find generally good agreement.",
"doi": "10.1007/978-0-387-74184-0_20",
"isbn": "9780387741833",
"publisher": "Springer New York",
"place_of_publication": "New York, NY",
"publication_date": "2007-05-25",
"pages": "195-205"
},
{
"id": "authors:5f29p-crk70",
"collection": "authors",
"collection_id": "5f29p-crk70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150324-133810503",
"type": "article",
"title": "Anomalous cosmic rays in the distant heliosphere and the reversal of the Sun's magnetic polarity in Cycle 23",
"author": [
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"abstract": "Beginning in early June 2001 and extending over a \u223c3 month period the Cosmic Ray Subsystem (CRS) experiment on Voyager 1 (80.3 AU, 34\u00b0N) observed a rapid transition in the energy of the peak intensity of anomalous cosmic ray (ACR) He from \u223c11 MeV/n to \u223c25 MeV/n. One month later there began a similar spectral shift at Voyager 2 (64.7 AU, 24\u00b0S). When these ACR transition times are extrapolated back from the estimated location of the heliospheric termination shock (TS) to the Sun (\u223c1 year) there is reasonable agreement with the range of times obtained for the polarity reversal of the interplanetary magnetic field (IPB) in the northern hemisphere near the Sun and the later reversal in the south. We interpret these changes in the ACR spectra as giving a global view of the interplanetary field reversal at the TS and confirmation of the important role of the TS in controlling the ACRs.",
"doi": "10.1029/2006GL028932",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "2007-03-07",
"series_number": "5",
"volume": "34",
"issue": "5",
"pages": "Art. No. L05105"
},
{
"id": "authors:rcex4-yx275",
"collection": "authors",
"collection_id": "rcex4-yx275",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150501-112052606",
"type": "book_section",
"title": "Primary and secondary contributions to arriving abundances of cosmic x-ray nuclides",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Ogliore",
"given_name": "R. C.",
"clpid": "Ogliore-R-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "The arriving abundances of a variety of cosmic-ray nuclides consist of comparable amounts of primary material produced by stellar nucleosynthesis and secondary matter resulting from fragmentation of heavier nuclei by collisions during interstellar propagation. We discuss a technique for extracting the primary and secondary contributions that takes advantage of energy spectra of individual nuclides\navailable from the Advanced Composition Explorer mission, a data base of measured and calculated fragmentation cross sections, and the leaky box model of interstellar propagation.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:xz7ge-1h388",
"collection": "authors",
"collection_id": "xz7ge-1h388",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150501-104753399",
"type": "book_section",
"title": "The High Energy Telescopes for the STEREO Mission",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Reames",
"given_name": "D. V.",
"clpid": "Reames-D-V"
},
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "We describe the High Energy Telescopes (HETs), which are part of the IMPACT investigation for the STEREO mission (Principal Investigator: Janet Luhmann, University of California atBerkeley). The two STEREO spacecraft were launched from Cape Canaveral, FL on October 25, 2006. High energy electrons (~ 0.7 -6 MeV) and nuclei from hydrogen to iron (~ 13 \u2013 200MeV/nucleon) are detected by the HETs, one on each spacecraft. Observations from one pass through the Earth's magnetosphere and from four X-class solar events in December, 2006 are presented to illustrate the capabilities of the HETs. The HET observations are also compared with observations from other spacecraft. The event of December 13th was the first Ground Level Event in almost two years.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:xg291-7mr32",
"collection": "authors",
"collection_id": "xg291-7mr32",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150501-111243485",
"type": "book_section",
"title": "Can ^(59)Ni Synthesized in OB Associations Decay to ^(59)Co Before Being Accelerated to Cosmic-ray Energies?",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "Observations from the Cosmic Ray Isotope Spectrometer (CRIS) aboard NASA's Advanced Composition Explorer (ACE) have shown that all relevant galactic cosmic-ray isotopic ratios measured are consistent with an OB-association origin of galactic cosmic rays (GCRs). Additionally\nCRIS measurements of the isotopic abundances of ^(59)Ni and ^(59)Co have shown that the 59Ni has completely decayed into ^(59)Co, indicating a delay of >10^5 years between nucleosynthesis and acceleration. However, it has been suggested that shocks generated from high-velocity Wolf-Rayet winds in the OB-association environment must accelerate nuclei synthesized in nearby core-collapse supernovae on a time scale short compared to the ^(59)Ni half-life of 7.6x10^4 years. If this were the case, it would\nimply that OB associations could not be the source of most galactic cosmic rays. In this paper, we describe the OB-association history and environment and show that the time scales for acceleration are such that most ^(59)Ni should be expected to decay naturally in that setting, strengthening the argument that OB associations are the likely source of a substantial fraction of galactic cosmic rays.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:8vb53-skh50",
"collection": "authors",
"collection_id": "8vb53-skh50",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150413-133110805",
"type": "book_section",
"title": "Observations of the December 2006 solar energetic particle events with the Low Energy Telescope (LET) on STEREO",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Looper",
"given_name": "M. L.",
"clpid": "Looper-M-L"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Miyasaka",
"given_name": "Hiromasa",
"orcid": "0000-0002-8074-4186",
"clpid": "Miyasaka-Hiromasa"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F.A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "NASA's Solar-Terrestrial Relations Observatory (STEREO) was launched in October 2006 carrying an advanced payload of imaging and in situ instrumentation designed to study coronal mass ejections and associated soalr energetic particle (SEP) events and interplanetary effects. Included in the payload is a Low Energy Telescope (LET) designed to measure SEP composition, energy spectra, and anisotropics. This paper describes the LET sensor and measurements of the large solar eruptions of December 2006. These unexpected events fortunately provided opportunities to test the LET hardware and software and to cross-calibrate the LETs and several near-Earth instruments.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:2c3nq-yjv76",
"collection": "authors",
"collection_id": "2c3nq-yjv76",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160722-135442634",
"type": "book_section",
"title": "Primary and secondary contributions to arriving abundances of cosmic-ray nuclides",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Ogliore",
"given_name": "R. C.",
"clpid": "Ogliore-R-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "Lukas",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sancehz-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "The arriving abundances of a variety of cosmic-ray nuclides consist of comparable amounts of primary material produced by stellar nucleosynthesis and secondary matter resulting from fragmentation of heavier nuclei by collisions during interstellar propagation. In order to utilize such species in studies of cosmic-ray source composition it is necessary to determine the secondary fraction present in the arriving material and to assess the uncertainty in this determination. We have extracted the primary and secondary contributions to the arriving abundances for isotopes of elements between B and Ni by using 1) measurements of cosmic-ray elemental and isotopic composition obtained from the Cosmic Ray Isotope Spectrometer (CRIS) instrument on the Advanced Composition Explorer (ACE) spacecraft, 2) a data base of measured and calculated fragmentation cross sections, and 3) a leaky box model of interstellar propagation. We present derived decompositions and discuss their implications for studies of the composition of cosmic-ray source material. This work was supported by NASA at Caltech (under grant NAG5-12929), JPL, Washington University, and GSFC.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:2xytk-zm886",
"collection": "authors",
"collection_id": "2xytk-zm886",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150415-153704362",
"type": "book_section",
"title": "Can ^(59)Ni Synthesized in OB Associations Decay to ^(59)Co Before Being Accelerated to Cosmic-ray Energies",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "Observations from the Cosmic Ray Isotope Spectrometer (CRIS) aboard NASA's Advanced Composition Explorer (ACE) have shown that all relevant galactic cosmic-ray isotopic ratios measured are consistent with an OB-association origin of galactic cosmic rays (GCRs). Additionally\nCRIS measurements of the isotopic abundances of ^(59)Ni and ^(59)Co have shown that the ^(59)Ni has completely decayed into ^(59)Co, indicating a delay of >105 years between nucleosynthesis and acceleration. However, it has been suggested that shocks generated from high-velocity Wolf-Rayet winds in the OB-association environment must accelerate nuclei synthesized in nearby core-collapse supernovae on a time scale short compared to the ^(59)Ni half-life of 7.6x10^4 years. If this were the case, it would\nimply that OB associations could not be the source of most galactic cosmic rays. In this paper, we describe\nthe OB-association history and environment and show that the time scales for acceleration are such that most ^(59)Ni should be expected to decay naturally in that setting, strengthening the argument that OB associations are the likely source of a substantial fraction of galactic cosmic rays.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:32hm9-1s478",
"collection": "authors",
"collection_id": "32hm9-1s478",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150501-110503078",
"type": "book_section",
"title": "Voyager observations of energetic particles near the solar wind termination shock",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "Voyager 1 is observing the energy spectra of anomalous cosmic ray H, He, and O in the heliosheath. The relative abundance of H/He is 20 at 1-1.5 MeV/nuc, indicating that H pickup ions are more efficiently accelerated than was modeled from observations at higher energies. Voyager 2 began observing upstream energetic ions from the shock in late 2004 at \u223c75 AU, about 10 AU closer to the Sun than observed by Voyager 1. Voyager 2 will be at 84.7 AU at the end of 2007 and may have crossed the termination shock.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:3apnk-px332",
"collection": "authors",
"collection_id": "3apnk-px332",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150422-162304614",
"type": "book_section",
"title": "Comparing observations and expectations of SEP composition in the two December 2006 events",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "In early December 2006, a large active region (number 10930) rotated over the eastern limb of the Sun. As it crossed the disk, it produced 4 X-class flares and at least 3 halo coronal mass ejections. Two large SEP events\n were generated when the region was at ~E70 and ~W25 and were observed by several spacecraft, including ACE and \nSTEREO. We have combined observations from the Solar Isotope Spectrometer (SIS) and the Ultra-Low Energy Isotope Spectrometer (ULEIS) on ACE and the Low Energy Telescope (LET) on STEREO for both SEP events. By integrating the SEP data over the duration of each event, the energy sp\nectra for many heavy ion species (including Mg, Si, and Ca) can be analyzed in detail and the elemental SEP composition can be compared for the two events. We find significant differences in the composition of the two events, with the second event having a high Fe/O ratio, similar to that of impulsive SEP events. Both events are examined in terms \nof expectations from two prevailing models, but neither model completely predicts the observations.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:d4xsd-d2v21",
"collection": "authors",
"collection_id": "d4xsd-d2v21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150422-161550254",
"type": "book_section",
"title": "Observations of corotating interaction regions from STEREO and ACE",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Miyasaka",
"given_name": "H.",
"orcid": "0000-0002-8074-4186",
"clpid": "Miyasaka-Hiromasa"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "Abstract: In the present declining phase of the solar cycle, corotating interaction regions (CIRs) have once again become more prevalent. Since the launch of the two STEREO spacecraft in October 2006, several significant recurring particle enhancements due to CIRs have been observed at 1 AU. The Low Energy Telescope (LET) on each STEREO spacecraft has been operating since mid-November 2006. This instrument is capable of measuring elemental composition and spectra for particles from H to Ni (and beyond) from \u223c2 to \u223c50 MeV/nucleon, depending on species, while the Suprathermal Ion Telescope (SIT) on STEREO measures ion composition from \u223c0.05 to 5 MeV/nucleon. Using data from these STEREO instruments, supplemented with measurements from ULEIS and SIS on ACE, we present preliminary observations of H, He, and heavy ion spectra and time profiles of the CIR events of 2007.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:d8jpm-hnh71",
"collection": "authors",
"collection_id": "d8jpm-hnh71",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150415-152222754",
"type": "book_section",
"title": "Persistent energetic ^3He in the inner heliosphere",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F.A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "Using data from the Solar Isotope Spectrometer on NASA's Advanced Composition Explorer spacecraft we have examined the time and energy dependence of the quiet-time 5\u201315 MeV/nuc He intensity from 1998 through 2006 in order to establish the origin of these particles. We find a mixed\npopulation, with He from impulsive solar energetic particle events dominating at the lower end of this energy interval and galactic secondary He becoming significant at the high end.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:psjf9-zta49",
"collection": "authors",
"collection_id": "psjf9-zta49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150416-150551459",
"type": "book_section",
"title": "Changing anomalous cosmic ray oxygen radial intensity gradients between 1 AU and Voyager with the return to solar minimum",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "Using the Solar Isotope Spectrometer (SIS) on NASA's ACE spacecraft, we have measured the intensities of anomalous cosmic rays (ACRs) near 1 AU down to energies of 10 MeV/nucleon since August 1997. As solar minimum modulation conditions return, ACR intensities at 1 AU are recovering,\nbut are significantly lower relative to galactic cosmic rays (GCRs) than they were during the intensity decline following the last solar minimum and are still a factor of 4 lower than in 1997. The large-scale radial intensity gradients of ACR oxygen obtained using observations from ACE, Voyagers 1 and 2, and Ulysses are much larger during the present A 0 recovery than they were during the last A 0 solar minimum;\nin fact beyond 50 AU ACR intensities already exceed those at the last A 0 solar minimum. The\n1 AU ACR measurements are now being augmented by data from the Low Energy Telescope (LET) on\nthe twin STEREO spacecraft, which will allow us to extend the energy spectra down to 3 MeV/nucleon\nto track the behavior of the peak of the ACR oxygen spectrum and study longitudinal intensity variations.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:k07mm-3fq74",
"collection": "authors",
"collection_id": "k07mm-3fq74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150414-113415014",
"type": "book_section",
"title": "Measurement of the Relative Abundances of the Ultra-Heavy Galactic Cosmic Rays (30 \u2264 Z \u2264 40) with TIGER",
"author": [
{
"family_name": "Rauch",
"given_name": "B. F.",
"clpid": "Rauch-B-F"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Barbier",
"given_name": "L. M.",
"clpid": "Barbier-L-M"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Geier",
"given_name": "S.",
"orcid": "0000-0002-3948-9339",
"clpid": "Geier-S"
},
{
"family_name": "Link",
"given_name": "J. T.",
"clpid": "Link-J-T"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mitchell",
"given_name": "J. W.",
"clpid": "Mitchell-J-W"
},
{
"family_name": "Schindler",
"given_name": "S. M.",
"clpid": "Schindler-S-M"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Streitmatter",
"given_name": "R. E.",
"clpid": "Streitmatter-R-E"
},
{
"family_name": "Waddington",
"given_name": "C. J.",
"clpid": "Waddington-C-J"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F.A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "Observations of ultra-heavy (Z\u226530) galactic cosmic rays (GCR) help to distinguish possible origins of GCR. The Trans-Iron Galactic Element Recorder (TIGER) measures the charge (Z) and energy of GCR using a combination of scintillators, Cherenkov detectors, and a scintillating fiber hodoscope. The two Cherenkov radiators, one acrylic\n and one aerogel, provide TIGER with an energy sensitivity between 0.3 and 10 GeV/nucleon in the instrument. The threshold at the top of the atmosphere is close to 0.8 GeV/nucleon for Fe. TIGER has accumulated data on two successful flights from McMurdo, Antarctica launched in D\necember 2001 and December 2003 with a total flight duration of 50 days. The combined dataset resolves ~140 nuclei with Z > 30, and provides the best measurements to date for \n30Zn, 31Ga, 32Ge, and 34Se. The results for Ga and Ge taken together are inconsistent with a GCR source with\n Solar-System abundances modified either by preferential acceleration of elements of low first ionization potential or by preferential acceleration of refractory elements, \nsuggesting that elemental composition of the GCR source is different from that of the Solar System",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:ktdsp-mae60",
"collection": "authors",
"collection_id": "ktdsp-mae60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150413-154918541",
"type": "book_section",
"title": "Cosmic-ray helium intensities over the solar cycle from ACE",
"author": [
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Lave",
"given_name": "K.",
"clpid": "Lave-K"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Moskalenko",
"given_name": "I. V.",
"clpid": "Moskalenko-I-V"
},
{
"family_name": "Ogliore",
"given_name": "R. C.",
"clpid": "Ogliore-R-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F.A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "Observations of cosmic-ray helium energy spectra provide important constraints on cosmic ray origin and propagation. However, helium intensities measured at Earth are affected by solar modulation, especially below several GeV/nucleon. Observations of helium intensities over a solar cycle are important for understanding how solar modulation affects galactic cosmic ray intensities and for separating the contributions of anomalous and galactic cosmic rays. The Cosmic Ray Isotope Spectrometer (CRIS) on ACE has been measuring cosmic ray isotopes, including helium, since 1997 with high statistical precision. We present helium elemental intensities between \u223c10 to \u223c100 MeV/nucleon from the Solar Isotope Spectrometer (SIS) and CRIS observations over a solar cycle and compare these results with the observations from other satellite and balloon-borne instruments, and with GCR transport and solar modulation models.",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:n9m2z-c2q35",
"collection": "authors",
"collection_id": "n9m2z-c2q35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150415-152910440",
"type": "book_section",
"title": "Possible role of transients on the energy spectra of energetic particles at the solar wind termination shock",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Caballero",
"given_name": "R.",
"clpid": "Cabalero-R"
},
{
"family_name": "D'Olivo",
"given_name": "J. C.",
"clpid": "D'Olivo-J-C"
},
{
"family_name": "Medina-Tanco",
"given_name": "G.",
"clpid": "Medina-Tanco-G"
},
{
"family_name": "Nellen",
"given_name": "L.",
"clpid": "Nellen-L"
},
{
"family_name": "Sanchez",
"given_name": "F. A.",
"clpid": "Sanchez-F-A"
},
{
"family_name": "Vald\u00e9s-Galicia",
"given_name": "J. F.",
"clpid": "Vald\u00e9s-Galicia-J-F"
}
],
"abstract": "We suggest that a series of merged interaction regions interacted with the solar wind termination\nshock for several years prior to its crossing by Voyager 1 in December 2004 and created the observed\nspectral shape of energetic particles. We also find that the charge-state of He with 3 to 70 MeV/nuc\nand O with 1 to 14 MeV/nuc is +1 and that the rigidity dependence of the diffusion coefficient from\n170 MV to 2.7 GV is given by .",
"publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico",
"publication_date": "2007"
},
{
"id": "authors:nyzka-vxa38",
"collection": "authors",
"collection_id": "nyzka-vxa38",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BINjpcs06",
"type": "article",
"title": "Superbubbles, Wolf-Rayet stars, and the origin of galactic cosmic rays",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"clpid": "Weidenbeck-M-E"
},
{
"family_name": "Arnould",
"given_name": "M.",
"clpid": "Arnould-M"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Goriely",
"given_name": "S.",
"clpid": "Goriely-S"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Meynet",
"given_name": "G.",
"clpid": "Meynet-G"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The abundances of neon and several other isotopic ratios in the galactic cosmic rays (GCRs) have been measured using data from the Cosmic Ray Isotope Spectrometer (CRIS) aboard the Advanced Composition Explorer (ACE). We have derived the 22Ne/20Ne ratio at the cosmic-ray source using the measured 21Ne, 19F, and 17O abundances as \"tracers\" of secondary isotope production. Using this approach, the 22Ne/20Ne abundance ratio obtained for the cosmic-ray source is 0.387 \u00b1 0.007 (stat.) \u00b1 0.022 (syst.). This corresponds to an enhancement by a factor of 5.3\u00b10.3 over the 22Ne/20Ne ratio in the solar wind. We compare our data for neon and refractory isotope ratios, and data from other experiments, with recent results from two-component Wolf-Rayet (WR) models. The three largest deviations of GCR isotope ratios from solar system ratios predicted by these models, 12C/16O, 22Ne/20Ne, and 58Fe/56Fe, are present in the GCRs. In fact, all of the isotope ratios that we have measured are consistent with a GCR source consisting of about 80% material with solar-system composition and about 20% of WR material. Since WR stars are evolutionary products of O and B stars, and most OB stars exist in OB associations that form superbubbles, the good agreement of these data with WR models suggests that superbubbles are the likely source of at least a substantial fraction of GCRs.",
"doi": "10.1088/1742-6596/47/1/008",
"issn": "1742-6596",
"publisher": "Journal of Physics: Conference Series",
"publication": "Journal of Physics: Conference Series",
"publication_date": "2006-12",
"volume": "47",
"pages": "68-77"
},
{
"id": "authors:nktpg-hyy18",
"collection": "authors",
"collection_id": "nktpg-hyy18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140407-091931371",
"type": "article",
"title": "Source and consequences of a large shock near 79 AU",
"author": [
{
"family_name": "Richardson",
"given_name": "J. D.",
"orcid": "0000-0003-4041-7540",
"clpid": "Richardson-J-D"
},
{
"family_name": "Liu",
"given_name": "Y.",
"clpid": "Liu-Y"
},
{
"family_name": "Wang",
"given_name": "C.",
"clpid": "Wang-C"
},
{
"family_name": "McComas",
"given_name": "D. J.",
"orcid": "0000-0001-6160-1158",
"clpid": "McComas-D-J"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Acuna",
"given_name": "M. H.",
"clpid": "Acuna-M-H"
},
{
"family_name": "Ness",
"given_name": "N. F.",
"clpid": "Ness-N-F"
}
],
"abstract": "In March 2006, Voyager 2 (V2) observed a large interplanetary (IP) shock near 79 AU followed by a merged interaction region (MIR). This shock is comparable to the shock observed by V2 at 65 AU in October 2001; these two shocks are the largest observed by V2 since 1991 when V2 was at 35 AU. This shock provides the first opportunity to compare the plasma structure in an IP shock and MIR with the energetic particle fluxes in the termination shock (TS) foreshock region. The flux of >0.5 MeV particles observed by V2 decreased after the shock; the shock and MIR probably pushed the TS outward so that the foreshock region moved outside the distance of V2. The >70 MeV cosmic ray ions decreased in the MIR, probably due to the reduced inward transport caused by the enhanced magnetic field. We model two possible sources of this shock, fast streams from polar coronal holes and coronal mass ejections (CMEs); these sources, when combined, provide a reasonable match to the V2 data.",
"doi": "10.1029/2006GL027983",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "2006-12",
"series_number": "23",
"volume": "33",
"issue": "23",
"pages": "Art. No. L23107"
},
{
"id": "authors:zan2e-rsh70",
"collection": "authors",
"collection_id": "zan2e-rsh70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-155626084",
"type": "article",
"title": "Correlation between energetic ion enhancements and heliospheric current sheet crossings in the outer heliosphere",
"author": [
{
"family_name": "Richardson",
"given_name": "J. D.",
"orcid": "0000-0003-4041-7540",
"clpid": "Richardson-J-D"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Kasper",
"given_name": "J. C.",
"orcid": "0000-0002-7077-930X",
"clpid": "Kasper-J-C"
},
{
"family_name": "Zhang",
"given_name": "M.",
"clpid": "Zhang-M"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Ness",
"given_name": "N. F.",
"clpid": "Ness-N-F"
},
{
"family_name": "Liu",
"given_name": "Y.",
"clpid": "Liu-Y"
}
],
"abstract": "Voyagers 1 and 2 observed highly-variable beams of energetic ions in the foreshock region upstream of the termination shock (TS). At Voyager 2 (V2), the ion intensities are generally not related to the plasma properties. At Voyager 1 (V1), the beams are often coincident with crossings of the heliospheric current sheet (HCS). The V1 intensity peaks occur when the HCS is crossed from negative to positive magnetic polarities and V1 is within a few AU of the TS. Two mechanisms are considered: current sheet drift and streaming of ions from the TS along magnetic field lines which are parallel to the HCS. The current sheet drift hypothesis predicts that enhancements observed at V2 will occur when the HCS is crossed in the opposite direction, from positive to negative magnetic polarity, since V2 is at southern heliolatitudes.",
"doi": "10.1029/2006GL027578",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "2006-11-14",
"series_number": "21",
"volume": "33",
"issue": "21",
"pages": "Art. No. L21112"
},
{
"id": "authors:kap4x-tqq13",
"collection": "authors",
"collection_id": "kap4x-tqq13",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110120-162201593",
"type": "article",
"title": "Wolf-Rayet stars, OB associations, and the origin\n of galactic cosmic rays",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Arnould",
"given_name": "M.",
"clpid": "Arnould-M"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Goriely",
"given_name": "S.",
"clpid": "Goriely-S"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Meynet",
"given_name": "G.",
"clpid": "Meynet-G"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "We have measured the isotopic abundances of neon and several refractory species in the galactic cosmic rays (GCRs) using the cosmic\nray isotope spectrometer (CRIS) aboard the ACE spacecraft. The ^(22)Ne/^(20)Ne ratio at the cosmic-ray source that we have obtained is\n0.387 \u00b1 0.007 (stat.) \u00b1 0.022 (syst.), which corresponds to enhancement by a factor of 5.3 \u00b1 0.3 over that in the solar wind. Our\nACE-CRIS data, and data from other experiments, are compared to recent results from two-component Wolf-Rayet (WR) models.\nThe three largest deviations of galactic cosmic ray isotope ratios from solar-system ratios predicted by these models, ^(12)C/^(16)O,^(22)Ne/^(20)Ne,\nand ^(58)Fe/^(56)Fe, are, in fact, very close to those observed. Furthermore, all of the isotope ratios that we have measured are consistent with\na GCR source consisting of ~20% of WR material mixed with ~80% material with solar-system composition. Since WR stars are evolutionary\nproducts of OB stars, and most OB stars exist in OB associations that form superbubbles, the good agreement of our data with\nWR models suggests that OB associations within superbubbles are the likely source of at least a substantial fraction of GCRs.",
"doi": "10.1016/j.newar.2006.06.058",
"issn": "1387-6473",
"publisher": "Elsevier",
"publication": "New Astronomy Reviews",
"publication_date": "2006-10",
"series_number": "7-8",
"volume": "50",
"issue": "7-8",
"pages": "516-520"
},
{
"id": "authors:zm2md-rb662",
"collection": "authors",
"collection_id": "zm2md-rb662",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:MCDaipcp06",
"type": "book_section",
"title": "Voyager observations of galactic and anomalous cosmic rays in the helioshealth",
"book_title": "PHYSICS OF THE INNER HELIOSHEATH: Voyager Observations, Theory, and Future Prospects; 5th Annual IGPP International Astrophysics Conference",
"author": [
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"contributor": [
{
"family_name": "Heerikhuisen",
"given_name": "Jacob"
},
{
"family_name": "Florinski",
"given_name": "Vladimir"
},
{
"family_name": "Zank",
"given_name": "Gary P."
},
{
"family_name": "Pogorelov",
"given_name": "Nikolai V."
}
],
"abstract": "Anomalous cosmic rays display large temporal variations at the time and location where Voyager 1 (V1) crossed the heliospheric termination shock (2004.86) (94AU, 34\u00b0N). On a short time scale (3 months) there was a large decrease produced by a series of merged interaction regions (MIR), the first of which was associated with the intense Oct./Nov. 2003 solar events. On a longer time scale there is a remarkable correlation between changes in the galactic cosmic ray (GCR) intensity and those of 10\u201356 MeV/n ACR He and 30\u201356 MeV H extending over a 4.3 year period with the GCRs exhibiting their expected behavior over this part of the 11 and 22 year solar activity and heliomagnetic cycle. The relative changes in the ACR and GCR are the same for both the short term and long term variations. The comparative V1/V2 ACR and GCR spectra in the foreshock and heliosheath indicate that at this time most of the higher energy ACRs are not being accelerated near V1 but must have their source region elsewhere \u2014 possibly near the equatorial region of the TS as was suggested in our first paper on the TS crossing (1).",
"doi": "10.1063/1.2359309",
"isbn": "978-0-7354-0355-0",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2006-09-26",
"pages": "79-85"
},
{
"id": "authors:5net5-e5e33",
"collection": "authors",
"collection_id": "5net5-e5e33",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090918-090238147",
"type": "book_section",
"title": "Termination shock particle spectral features",
"book_title": "Physics of the Inner Heliosheath: Voyager Observations, Theory, and Future Prospects; 5th Annual IGPP International Astrophysics Conference",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Heerikhuisen",
"given_name": "Jacob",
"clpid": "Heerikhuisen-J"
},
{
"family_name": "Florinksi",
"given_name": "Vladimir",
"clpid": "Florinski-V"
},
{
"family_name": "Zank",
"given_name": "Gary P.",
"clpid": "Zank-G-P"
},
{
"family_name": "Pogorelov",
"given_name": "Nikolai V.",
"clpid": "Pogorelov-N-V"
}
],
"abstract": "Spectral features of energetic H ions accelerated at the termination shock may be evidence of two components. At low energies the energy spectrum is ~E^(\u20131.55), with break at ~0.4 MeV to E^(\u20132.2). A second component appears above ~1 MeV with a spectrum of E^(\u20131.27) with a break at ~3.2 MeV. Even though the intensities upstream are highly variable, the same spectral break energies are observed, suggesting that these are durable features of the source spectrum. The acceleration processes for the two components may differ, with the lower energy component serving as the injection source for diffusive shock acceleration of the higher energy component. Alternatively, the spectral features may result from the energy dependence of the diffusion tensor that affects the threshold for diffusive shock acceleration.",
"doi": "10.1063/1.2359310",
"isbn": "978073540355-0",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2006-09-26",
"pages": "86-91"
},
{
"id": "authors:dhn00-s9g22",
"collection": "authors",
"collection_id": "dhn00-s9g22",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140407-093553418",
"type": "article",
"title": "The disappearance of anomalous protons at Voyager 1 and Voyager 2 in the outer heliosphere between 1998 and 2002",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"abstract": "In 1998 and 1999 at V1 and V2 in the outer heliosphere between 55 and 75 AU, large intensities of anomalous H were observed with a peak in the differential energy spectrum at \u223c25 MeV. Subsequently, in 2000 and 2001 when these spacecraft were 5\u201310 AU further out, these intensities were greatly reduced by 11-year modulation effects, so that by the beginning of 2002 anomalous H had completely disappeared beneath the E^(1.0) spectrum of galactic H at low energies. The modulation between 1998 and 2002 produced intensity changes of galactic H similar to those observed at the Earth in the same time period except that the changes at V1 and V2 were much smaller. The intensity change at V2 was also larger than that at V1. For anomalous H, however, the intensity changes at V1 and V2 were a factor of 10\u201320 times larger than those for galactic H, so that by the end of 2001 the anomalous H intensities were less than 1% of their 1998 values. Also, during one time period in late 2001 there was a large reduction of anomalous H at both V1 and V2 with no corresponding change in galactic H. These different intensity changes between galactic and anomalous H provide an insight into particle transport, drift, and acceleration processes in the region near the heliospheric termination shock, which is located just beyond V1. Radial gradient comparisons in 1998 and also at the times of reduced anomalous H intensities imply that most of the intensity reduction of anomalous H apparently occurred at \u223c90 AU or beyond. This could indicate source changes in the anomalous H spectra but most likely is a measure of changes in the \"connection\" between V1 and V2 and the source region, such as might be caused by changing drift patterns and particle entry into the heliosphere.",
"doi": "10.1029/2006JA011669",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2006-08-26",
"series_number": "A8",
"volume": "111",
"issue": "A8",
"pages": "Art. No. A08107"
},
{
"id": "authors:dc38s-4x526",
"collection": "authors",
"collection_id": "dc38s-4x526",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-093644016",
"type": "article",
"title": "Cosmic-Ray Neon, Wolf-Rayet Stars, and the Superbubble Origin of Galactic Cosmic Rays",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Arnould",
"given_name": "M.",
"clpid": "Arnould-M"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Goriely",
"given_name": "S.",
"clpid": "Goriely-S"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Meynet",
"given_name": "G.",
"clpid": "Meynet-G"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "We report the abundances of neon isotopes in the Galactic cosmic rays (GCRs) using data from the Cosmic Ray Isotope Spectrometer (CRIS) aboard the Advanced Composition Explorer (ACE). These abundances have been measured for seven energy intervals over the energy range of 84 \u2264 E/M \u2264 273 MeV nucleon^(-1). We have derived the ^(22)Ne/^(20)Ne ratio at the cosmic-ray source using the measured ^(21)Ne, ^(19)F, and ^(17)O abundances as \"tracers\" of secondary production of the neon isotopes. Using this approach, the ^(22)Ne/^(20)Ne abundance ratio that we obtain for the cosmic-ray source is 0.387 \u00b1 0.007(statistical) \u00b1 0.022(systematic). This corresponds to an enhancement by a factor of 5.3 \u00b1 0.3 over the ^(22)Ne/^(20)Ne ratio in the solar wind. This cosmic-ray source ^(22)Ne/^(20)Ne ratio is also significantly larger than that found in anomalous cosmic rays, solar energetic particles, most meteoritic samples of matter, and interplanetary dust particles. We compare our ACE CRIS data for neon and refractory isotope ratios, and data from other experiments, with recent results from two-component Wolf-Rayet (W-R) models. The three largest deviations of GCR isotope ratios from solar system ratios predicted by these models, ^(12)C/^(16)O, ^(22)Ne/^(20)Ne, and ^(58)Fe/^(56)Fe, are indeed present in the GCRs. In fact, all of the isotope ratios that we have measured are consistent with a GCR source consisting of about 80% material with solar system composition and about 20% W-R material. Since W-R stars are evolutionary products of OB stars, and most OB stars exist in OB associations that form superbubbles, the good agreement of these data with W-R models suggests that superbubbles are the likely source of at least a substantial fraction of GCRs.",
"doi": "10.1086/496959",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2005-11-20",
"series_number": "1",
"volume": "634",
"issue": "1",
"pages": "351-364"
},
{
"id": "authors:rb184-jnt10",
"collection": "authors",
"collection_id": "rb184-jnt10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-084449577",
"type": "article",
"title": "Voyager 1 Explores the Termination Shock Region and the Heliosheath Beyond",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "Voyager 1 crossed the termination shock of the supersonic flow of the solar wind on 16 December 2004 at a distance of 94.01 astronomical units from the Sun, becoming the first spacecraft to begin exploring the heliosheath, the outermost layer of the heliosphere. The shock is a steady source of low-energy protons with an energy spectrum \u223cE^(\u20131.41 \u00b1 0.15) from 0.5 to \u223c3.5 megaelectron volts, consistent with a weak termination shock having a solar wind velocity jump ratio r = 2.6^(+0.4)_(-0.2). However, in contradiction to many predictions, the intensity of anomalous cosmic ray (ACR) helium did not peak at the shock, indicating that the ACR source is not in the shock region local to Voyager 1. The intensities of \u223c10\u2013megaelectron volt electrons, ACRs, and galactic cosmic rays have steadily increased since late 2004 as the effects of solar modulation have decreased.",
"doi": "10.1126/science.1117684",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "2005-09-23",
"series_number": "5743",
"volume": "309",
"issue": "5743",
"pages": "2017-2020"
},
{
"id": "authors:459jm-wtt31",
"collection": "authors",
"collection_id": "459jm-wtt31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140407-101736587",
"type": "article",
"title": "Heavy ion abundances and spectra from the large solar energetic particle events of October-November 2003",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008",
"clpid": "Desai-M-I"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "Observations from the Solar Isotope Spectrometer and the Ultra Low Energy Isotope Spectrometer on the ACE spacecraft during the extremely large events of October and November 2003 are combined to create heavy ion spectra over more than 3 decades in energy. The resulting spectra differed substantially in shape from event to event, as well as from element to element within a given event, resulting in energy-dependent abundance ratios. Although the effects of strong local shock acceleration are apparent in the intensities of the 28 and 29 October events, these do not explain the order of magnitude differences between the event-integrated abundances obtained at 0.64\u20130.91 MeV/nucleon and those at 12\u201360 MeV/nucleon. The higher-energy abundances relative to the lower-energy ones show trends with nuclear charge or charge-to-mass ratio that are similar for all the events and suggest that heavier ions are less efficiently accelerated to high energies. The position of the breaks in the energy spectra of O, Ne, Mg, Si, S, Ca, and Fe can be understood in terms of leakage from the shock region, if the mean free path is assumed to be a power law in rigidity. The resulting rigidity dependence is consistent with a source of wave turbulence in the vicinity of the shock when the ions are accelerated.",
"doi": "10.1029/2005JA011004",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2005-08-10",
"series_number": "A9",
"volume": "110",
"issue": "A9",
"pages": "Art. No. A09S16"
},
{
"id": "authors:p8g9y-hq698",
"collection": "authors",
"collection_id": "p8g9y-hq698",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110825-074422914",
"type": "book_section",
"title": "Solar Energetic Particle Spectral Breaks",
"book_title": "Physics of Collisionless Shocks",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Looper",
"given_name": "M. L.",
"clpid": "Looper-M-L"
},
{
"family_name": "Haggerty",
"given_name": "D. E.",
"clpid": "Haggerty-D-E"
},
{
"family_name": "Maclennan",
"given_name": "C. G.",
"clpid": "Maclennan-C-G"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008",
"clpid": "Desai-M-I"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Li",
"given_name": "G.",
"orcid": "0000-0001-9313-251X",
"clpid": "Li-Gang"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Li",
"given_name": "G.",
"clpid": "Li-Gang"
},
{
"family_name": "Zank",
"given_name": "G. P.",
"clpid": "Zank-G-P"
},
{
"family_name": "Russell",
"given_name": "C. T.",
"clpid": "Russell-C-T"
}
],
"abstract": "The five large solar particle events during October\u2013November 2003 presented an opportunity to test shock acceleration models with in-situ observations. We use solar particle spectra of H to Fe ions, measured by instruments on ACE, SAMPEX, and GOES-11, to investigate the Q/M-dependence of spectral breaks in the 28 October 2003 event. We find that the break energies scale as (Q/M)^b with b \u2248 1.56 to 1.75, somewhat less than predicted. We also conclude that SEP spectra >100 MeV/nucleon are best fit by a double power-law shape. \u00a92005 American Institute of Physics",
"doi": "10.1063/1.2032701",
"isbn": "0-7354-0268-X",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2005-08-01",
"pages": "227-232"
},
{
"id": "authors:6hw17-tsh44",
"collection": "authors",
"collection_id": "6hw17-tsh44",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110822-080338809",
"type": "book_section",
"title": "Observations of Energetic Ions and Electrons in the Distant Heliosphere: 2001 \u2013 2005.0",
"book_title": "The physics of collisionless shocks",
"author": [
{
"family_name": "McDonald",
"given_name": "Frank B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Burlaga",
"given_name": "Leonard F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "Bryant C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "Nand",
"clpid": "Lal-Nand"
},
{
"family_name": "Ness",
"given_name": "Norman F.",
"clpid": "Ness-N-F"
},
{
"family_name": "Richardson",
"given_name": "John D.",
"orcid": "0000-0003-4041-7540",
"clpid": "Richardson-J-D"
},
{
"family_name": "Webber",
"given_name": "William R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Li",
"given_name": "G.",
"clpid": "Li-Gang"
},
{
"family_name": "Zank",
"given_name": "G. P.",
"clpid": "Zank-G-P"
},
{
"family_name": "Russell",
"given_name": "C. T.",
"clpid": "Russell-C-T"
}
],
"abstract": "As Voyager 1 (V1) moves closer to the heliospheric termination shock (TS), a new energetic particle population is observed: Termination Shock Particle events (TSP). Interplanetary disturbances in the form of merged interaction regions (MIRs) \u2014 identified using Voyager 2 (V2) data \u2014 have a major effect on the V1 TSP events from their onset to termination along with triggering episodic increases in higher energy ions (35 MeV H) and MeV electrons. The nature of these interactions appear to evolve as V1 moves closer to the TS.",
"doi": "10.1063/1.2032706",
"isbn": "0-7354-0268-X",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2005-08-01",
"pages": "261-266"
},
{
"id": "authors:jg03k-ckt17",
"collection": "authors",
"collection_id": "jg03k-ckt17",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090918-084737847",
"type": "book_section",
"title": "Characteristics of the Termination Shock: Insights from Voyager",
"book_title": "The Physics of Collisionless Shocks: 4th Annual IGPP International Astrophysics Conference",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Li",
"given_name": "Gang",
"clpid": "Li-Gang"
},
{
"family_name": "Zank",
"given_name": "Gary P.",
"clpid": "Zank-G-P"
},
{
"family_name": "Russell",
"given_name": "C. T.",
"clpid": "Russell-C-T"
}
],
"abstract": "We examine the energy spectra obtained from the cosmic ray instrument on the Voyager 1 spacecraft during 2002/215 through 2005/60. We find that the energy spectra of protons below ~20 MeV often resemble two power laws with a relatively hard index at low energies and a softer index at higher energies. The point of intersection of the two power laws is ~3 MeV. Beginning in 2005, the low-energy index is typically \u20131.5, corresponding to a shock strength (compression ratio) of 2.5. We attribute these characteristics to a restricted region of the solar wind termination shock that is sporadically connected to the Voyager 1 spacecraft by the interplanetary magnetic field. The absence of significant spectral variability in 2005 suggests that Voyager 1 entered a region with minimal spatial gradients of the lowest energy ions.",
"doi": "10.1063/1.2032708",
"isbn": "073540268X",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2005-08-01",
"pages": "273-277"
},
{
"id": "authors:xp7nb-pzr89",
"collection": "authors",
"collection_id": "xp7nb-pzr89",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150324-090430351",
"type": "article",
"title": "Differences in the spectra of anomalous cosmic ray helium nuclei in two solar magnetic polarity cycles",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
}
],
"abstract": "We compare the spectra of anomalous He nuclei measured in the heliosphere by the IMP, Voyager, and Pioneer spacecraft at heliospheric distances ranging from 1 to over 80 AU in the time period from 1977 to 2003. Striking differences in the energy spectra of these nuclei are found between positive and negative solar magnetic polarity cycles. These differences are such that the spectra observed in negative polarity cycles appear to be greatly deficient in particles with energies of less than \u223c15 MeV but have an excess intensity above >25 MeV, relative to the spectra observed in positive cycles. These spectral differences are complex and may be related to both solar modulation effects inside of the heliospheric termination shock as well as differences occurring at or near the termination shock itself. At the modulation minimum in 1998 when V2 was at a distance of 56 AU and V1 at 71 AU, a high intensity of low-energy anomalous He particles was observed with a peak in the spectrum at \u223c5 MeV/nuc. In late 2001 after the solar magnetic polarity had changed from positive to negative and the 11-year solar modulation had increased, the previous high intensities of the anomalous He nuclei seen in 1998 were greatly reduced at both V1 and V2, and the energy of the peak intensity had moved up to \u223c20\u201325 MeV/nuc. However, in both polarity periods the highest-energy part of this spectrum above \u223c30 MeV/nuc is similar with a slope of \u22122.8 \u00b1 0.2. The details of these complex spectral changes are described in this paper.",
"doi": "10.1029/2005JA011123",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2005-07-27",
"series_number": "A7",
"volume": "110",
"issue": "A7",
"pages": "Art. No. A07106"
},
{
"id": "authors:8fq5g-pz718",
"collection": "authors",
"collection_id": "8fq5g-pz718",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-114144077",
"type": "article",
"title": "Isotopic Composition of Cosmic Rays: Results from the Cosmic Ray Isotope Spectrometer on the ACE Spacecraft",
"author": [
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "The Cosmic Ray Isotope Spectrometer on the ACE spacecraft measures the isotopic composition of cosmic-ray elements from Li through Zn with an unprecedented combination of excellent mass resolution and high statistics. The results indicate a cosmic-ray source whose composition is remarkably similar to that of the solar system, but which is enriched in material that may have originated in Wolf-Rayet stars. The lack of ^(59)Ni is strong indication that the cosmic rays are accelerated at least 10^5 years after nucleosynthesis. We examine these results in the context of the superbubble model of cosmic-ray origin that has been described by Higdon and Lingenfelter.",
"doi": "10.1016/j.nuclphysa.2005.05.038",
"issn": "0375-9474",
"publisher": "Elsevier",
"publication": "Nuclear Physics A",
"publication_date": "2005-07-25",
"volume": "758",
"pages": "201-208"
},
{
"id": "authors:rhfjf-6s679",
"collection": "authors",
"collection_id": "rhfjf-6s679",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-135112110",
"type": "book_section",
"title": "Extended Energy Elemental Spectrum Measurements with the Solar Isotope Spectrometer (SIS)",
"author": [
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "The Solar Isotope Spectrometer (SIS) aboard the Advanced Composition Explorer (ACE) has been\nmeasuring solar energetic particle abundances since ACE was launched in August 1997. SIS is a silicon\ndetector telescope that identifies charged particles via the multiple dE/dx vs. total energy technique, and to\ndate, most measurements reported by SIS have been limited in energy to those particles that stop in the\ninstrument. In this paper, we will summarize the multiple dE/dx technique used to identify particles that\npenetrate through the bottom of SIS, extending the energy ranges for elemental abundance measurements.\nIn preliminary analysis, the upper energy limit for oxygen has been extended from ~90 MeV/nuc for\nstopping particles to ~300 MeV/nuc for penetrating particles, and the upper energy limit for iron has been\nextended from ~168 MeV/nuc to ~500 MeV/nuc. We apply this technique to SIS measurements of large SEP\nevents, such as the Nov. 6, 1997 event and the recent Jan. 20, 2005 event, to extend the measured spectra, to\nlook for evidence of spectral breaks.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:shahn-emn48",
"collection": "authors",
"collection_id": "shahn-emn48",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140902-084251924",
"type": "book_section",
"title": "Characteristics of the Solar Wind Termination Shock Region from Voyager 1 Observations",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "The Voyager 1 spacecraft crossed the solar wind termination shock on 16 December 2004 at a distance of\n94.0 AU from the Sun and at a heliolatitude of 34 N. Up to that time, since mid-2002, Voyager 1 had been\non interplanetary magnetic field lines intermittently connected to a source of low-energy particles at the\ntermination shock. The energy spectra after the crossing, and often prior to the crossing as well, resemble the\nenergy spectra expected for anomalous cosmic rays (ACRs) at the shock, with one important difference.\nAlthough the spectra have a power-law dependence at low energies and a roll off to a much steeper power-law\nspectrum at higher energies, similar to that expected for the ACR spectrum at the shock, the energy of\nthe roll off is much lower than observed in the ACR spectrum at the same time. Hence, the ACRs must be\noriginating from a different part of the shock. We find that the roll-off energy for protons is about 3 MeV,\nrather than ~100 MeV expected for ACR protons. The power-law spectral index at low energies is\napproximately \u20131.5, implying a shock strength of ~2.5.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:effh6-t9k64",
"collection": "authors",
"collection_id": "effh6-t9k64",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-135634611",
"type": "book_section",
"title": "Ultra-Heavy Elements Above 10 MeV/nucleon in Solar Energetic Particle Events",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Recent measurements from Wind/LEMT and ACE/ULEIS show that elements heavier than Zn (Z=30) can be enhanced by factors of ~100 to 10,000 in impulsive solar energetic particle (SEP) events at energies below several MeV/nuc. Using data from the Solar Isotope Spectrometer (SIS) on ACE at energies from ~10 to >100 MeV/nuc, we find that even large gradual events at these energies often are very iron rich and may appear similar in composition to impulsive events. Since August 1997, SIS has recorded ~1000 nuclei with Z\nof 29 or greater, including measurable quantities of Zn, Ge and Se (Z=30, 32, and 34). Although quantitative analysis to obtain ultra-heavy abundances remains to be done, we present sample observations that establish the potential of extending ultra-heavy SEP measurements up to higher energies in order to test models of\nacceleration and abundance enhancements in both gradual and impulsive events.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:hhtja-61w39",
"collection": "authors",
"collection_id": "hhtja-61w39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-092815858",
"type": "book_section",
"title": "Evidence for two energetic particle sources at the termination shock",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "During the period of unusual enhancements in the intensities of low energy ions observed by Voyager 1\nbeyond 85 AU, the energy spectra appear to have two components. Upstream of the termination shock, low\nenergy ions (<10 MeV/nucleon) stream along the magnetic field and have significant variations in intensity\nand spectral slope. Their power law spectrum often shows no evidence of modulation at the lowest energies.\nThis suggests a nearby source region of termination shock particles (TSPs) connected to Voyager along the\ninterplanetary magnetic field. At intermediate energies ( ~ 10 to 60 Me V /nucleon), the helium spectrum is\nrelatively steady and consistent with that of anomalous cosmic rays (ACRs) with modulation increasing with\ndecreasing energy. This indicates that the ACR source is a remote region of the termination shock not\nconnected to Voyager along the magnetic field. This distinction between the TSP and ACR sources was\nconfirmed when Voyager 1 crossed the termination shock at 94 AU.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:y72v2-bm013",
"collection": "authors",
"collection_id": "y72v2-bm013",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-134905200",
"type": "article",
"title": "IMPACT: Science goals and firsts with STEREO",
"author": [
{
"family_name": "Luhmann",
"given_name": "J. G.",
"orcid": "0000-0003-0626-9353",
"clpid": "Luhmann-J-G"
},
{
"family_name": "Cummings",
"given_name": "A.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Davis",
"given_name": "A.",
"clpid": "Davis-A"
}
],
"abstract": "The in situ measurements of particles and CME transients (IMPACT) investigation on the twin STEREO spacecraft focuses on the solar energetic particle, solar wind and suprathermal electron, and magnetic field measurements needed to address STEREO's goals. IMPACT will provide regular, identical, in situ multipoint measurements bracketing Earth as each spacecraft separates from it at a rate of \u223c22\u00b0/yr along Earth's orbit. Combined with the PLASTIC and SWAVES investigations, IMPACT fills a critical role in the STEREO quest to connect SECCHI's 3D coronal images to their interplanetary consequences.",
"doi": "10.1016/j.asr.2005.03.033",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "2005",
"series_number": "8",
"volume": "36",
"issue": "8",
"pages": "1534-1543"
},
{
"id": "authors:dtd12-ydn98",
"collection": "authors",
"collection_id": "dtd12-ydn98",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150409-092051213",
"type": "book_section",
"title": "The Level of Solar Modulation of Galactic Cosmic Rays from 1997 to 2005 as Derived from ACE Measurements of Elemental Energy Spectra",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Davis",
"given_name": "Mark E.",
"clpid": "Davis-M-E-Astro"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Acharya",
"given_name": "B.",
"clpid": "Acharya-B"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Jain",
"given_name": "Atul",
"clpid": "Jain-A"
},
{
"family_name": "Karthikeyan",
"given_name": "S.",
"clpid": "Karthikeyan-S"
},
{
"family_name": "Morris",
"given_name": "S.",
"clpid": "Morris-S"
},
{
"family_name": "Tonwar",
"given_name": "S.",
"clpid": "Tonwar-S"
}
],
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:kzkxf-3jv31",
"collection": "authors",
"collection_id": "kzkxf-3jv31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150409-094600102",
"type": "book_section",
"title": "Voyager 1 Observations of Termination Shock Particle Events \u2013 The Effect of Interplanetary Transients",
"author": [
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Acharya",
"given_name": "B.",
"clpid": "Acharya-B"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Jain",
"given_name": "Atul",
"clpid": "Jain-A"
},
{
"family_name": "Karthikeyan",
"given_name": "S.",
"clpid": "Karthikeyan-S"
},
{
"family_name": "Morris",
"given_name": "S.",
"clpid": "Morris-S"
},
{
"family_name": "Tonwar",
"given_name": "S.",
"clpid": "Tonwar-S"
}
],
"abstract": "The increases in MeV ions and electrons, observed by the Voyager 1 CRS experiment as it moved beyond\n85 AU, have persisted over most of the ensuing 3 year period and represents a new particle population in the\ndistant heliosphere - Termination Shock Particle (TSP) events. The properties of these TSP events are\nstrongly influenced by the passage of interplanetary transients.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:mjxec-bwj66",
"collection": "authors",
"collection_id": "mjxec-bwj66",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150409-093457645",
"type": "book_section",
"title": "Voyager 2 Observations of MeV Ions in the Outer Heliosphere Over the Solar Maximum Period of Cycle 23",
"author": [
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Ness",
"given_name": "N. F.",
"clpid": "Ness-N-F"
},
{
"family_name": "Richardson",
"given_name": "J. D.",
"orcid": "0000-0003-4041-7540",
"clpid": "Richardson-J-D"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Acharya",
"given_name": "B.",
"clpid": "Acharya-B"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Jain",
"given_name": "Atul",
"clpid": "Jain-A"
},
{
"family_name": "Karthikeyan",
"given_name": "S.",
"clpid": "Karthikeyan-S"
},
{
"family_name": "Morris",
"given_name": "S.",
"clpid": "Morris-S"
},
{
"family_name": "Tonwar",
"given_name": "S.",
"clpid": "Tonwar-S"
}
],
"abstract": "Over the period 2001.0 - 2005.4, (63 - 74 AU) Voyager 2 observed a series of 9 energetic particle increases\nthat persist over some 3 - 4 solar rotations, occur with a quasi-periodicity of some 145 days and are generally\nassociated with the passage of a merged interaction region. With the onset of GCR recovery from solar\nmaximum levels in 2004.6 there is a marked change in the nature of the V2 energetic particle increases that\nsuggest these new events originated at the termination shock.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:tzq5m-5s364",
"collection": "authors",
"collection_id": "tzq5m-5s364",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150406-161740226",
"type": "book_section",
"title": "The Time Variation of Energetic ^3He in Interplanetary Space from 1997-2005",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Gold",
"given_name": "R. E.",
"clpid": "Gold-R-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Acharya",
"given_name": "B.",
"clpid": "Acharya-B"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Jain",
"given_name": "Atul",
"clpid": "Jain-A"
},
{
"family_name": "Karthikeyan",
"given_name": "S.",
"clpid": "Karthikeyan-S"
},
{
"family_name": "Morris",
"given_name": "S.",
"clpid": "Morris-S"
},
{
"family_name": "Tonwar",
"given_name": "S.",
"clpid": "Tonwar-S"
}
],
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:8bdps-bv587",
"collection": "authors",
"collection_id": "8bdps-bv587",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140903-084303356",
"type": "book_section",
"title": "Solar Energetic Particle Spectra and Composition in the\n October/November 2003 Events",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008",
"clpid": "Desai-M-I"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "The series of extremely large solar energetic particle (SEP) events of October and November 2003 were well\nobserved by many spacecraft. We have combined data from the ULEIS and SIS instruments on ACE to\nobtain particle intensities over >3 decades in energy. The event-integrated composition (carbon through\niron) not only varies from event to event, but also as a function of energy within an SEP event. These\ncompositional variations are a result of the element-dependent spectral breaks and we suggest they can be\nsubstantially reduced when the spectra are examined in terms of rigidity-dependent escape from the shock.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:awt8h-59x26",
"collection": "authors",
"collection_id": "awt8h-59x26",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150406-154528900",
"type": "book_section",
"title": "Solar-Particle Energy Spectra during the Large Events of October-November 2003 and January 2005",
"author": [
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Acharya",
"given_name": "B.",
"clpid": "Acharya-B"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Jain",
"given_name": "Atul",
"clpid": "Jain-A"
},
{
"family_name": "Karthikeyan",
"given_name": "S.",
"clpid": "Karthikeyan-S"
},
{
"family_name": "Morris",
"given_name": "S.",
"clpid": "Morris-S"
},
{
"family_name": "Tonwar",
"given_name": "S.",
"clpid": "Tonwar-S"
}
],
"abstract": "The Solar Isotope Spectrometer (SIS) aboard the Advanced Composition Explorer (ACE) has beeo measuring solar energetic particle abundances since ACE was launched in August 1997. SIS is a silicon detector telescope that identifies charged particles via the multiple dE/dx vs. total energy technique, and to date, most measurements reported by SIS have beeo limited in energy to those particles that stop in the instrument. Io this paper, we will summarize the multiple dE/dx techoique used to identify particles that penetrate through the bottom of SIS, extending the energy ranges for elemental abundance measurements. Io preliminary analysis, the upper energy limit for oxygen has beeo extended from -90 MeV/nuc for\nstopping particles to -300 MeV/nuc for penetrating particles, and the upper energy limit for iron has beeo\nextended from -l 6S MeV /nuc to -500 MeV /nuc. We apply this techoique to SIS measurements oflarge SEP\nevents, such as the Nov. 6, 1997 event and the recent Jan. 20, 2005 event, to extend the measured spectra, to\nlook for evidence of spectral breaks.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:bfcd4-0xy36",
"collection": "authors",
"collection_id": "bfcd4-0xy36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140903-072308449",
"type": "book_section",
"title": "Intensity Gradients of Anomalous Cosmic Rays Between 1 AU and Voyager During Solar Cycle 23",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Using ACE/SIS data we obtain measurements of the variation of the anomalous cosmic ray (ACR) O intensity\nat 1 AU throughout the solar cycle, including periods near solar maximum. After being suppressed by a factor\nof ~100 or more from 2001 through 2003 during solar maximum, ACR intensities are once again recovering\nat 1 AU, but their intensities are lower relative to higher rigidity galactic cosmic rays (GCRs) than they were\nduring entry into solar maximum in 1998-2000. Comparison of the 1 AU ACR and GCR time variations with\nthose measured by both Voyager spacecraft in the outer heliosphere shows that both ACR and GCR large-scale\nradial gradients are greater at solar maximum than at solar minimum, and that the ACR radial gradients are\nmuch larger than those of the GCRs, becoming very large inside of ~5 AU.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:ap5c2-zwd26",
"collection": "authors",
"collection_id": "ap5c2-zwd26",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-093513358",
"type": "book_section",
"title": "Appearance of a Third Episode of Enhanced Particle Intensities at 94 AU: Voyager 1 in the Heliosheath",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "The Voyager 1 spacecraft crossed the solar wind termination shock on 16 December 2004 at 94.0 AU and\nbegan observing a new episode of enhanced intensities of termination shock particles (TSPs) in the\nheliosheath. Two earlier TSP episodes were observed upstream of the shock beginning in mid-2002 at 84\nAU as Voyager 1 and the shock were moving outward together. The upstream TSPs exhibited strong field-aligned\nbeaming and large spectral variability on a daily time scale that likely resulted from variations in the\nconnectivity of Voyager 1 to the source at the shock. In the heliosheath the TSP intensity and spectra are\nmuch less variable and the field aligned streaming greatly reduced, consistent with more uniform\npropagation conditions and a stable source intensity. The gradual evolution of the of the TSP and ACR\nspectra as Voyager l moves further beyond the shock should reveal new aspects of the heliosheath and\nacceleration of TSPs and ACRs.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "2005"
},
{
"id": "authors:44axx-tcn70",
"collection": "authors",
"collection_id": "44axx-tcn70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111004-094736990",
"type": "book_section",
"title": "Cosmic-Ray Spectra in Interstellar Space",
"book_title": "Physics of the outer heliosphere",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Florinski",
"given_name": "Vladimir",
"clpid": "Florinski-V"
},
{
"family_name": "Pogorelov",
"given_name": "Nikolai V.",
"clpid": "Pogorelov-N-V"
},
{
"family_name": "Zank",
"given_name": "G. P.",
"clpid": "Zank-G-P"
}
],
"abstract": "At energies below ~300 MeV/nuc our knowledge of cosmic-ray spectra outside the heliosphere is obscured by the energy loss that cosmic rays experience during transport through the heliosphere into the inner solar system. This paper compares measurements of secondary electron-capture isotope abundances and cosmic-ray spectra from ACE with a simple model of interstellar propagation and solar modulation in order to place limits on the range of interstellar spectra that are compatible with both sets of data.",
"doi": "10.1063/1.1809509",
"isbn": "0-7354-0199-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2004-09-15",
"pages": "127-132"
},
{
"id": "authors:rn5wk-ymk92",
"collection": "authors",
"collection_id": "rn5wk-ymk92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110830-093038896",
"type": "book_section",
"title": "The Energetic Particle Populations of the Distant\n Heliosphere",
"book_title": "Physics of the Outer Heliosphere",
"author": [
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Florinski",
"given_name": "Vladimir",
"clpid": "Florinski-V"
},
{
"family_name": "Pogorelov",
"given_name": "Nikolai V.",
"clpid": "Pogorelov-N-V"
},
{
"family_name": "Zank",
"given_name": "G. P.",
"clpid": "Zank-G-P"
}
],
"abstract": "In late 2003 as Voyager 1 moves beyond 90 AU in the recovery phase of solar cycle 23, the effects of the termination shock (TS) and the heliosheath on particle transport are becoming more evident. There are\nnow detectable fluxes of 2.5 \u2013 70 MeV electrons but at low intensity levels that suggest they are heavily modulated in the heliosheath. The modulation of galactic and anomalous cosmic rays is significant but much smaller than observed at 1 AU. At V1 a large increase of MeV ions was observed with a flat energy spectra which persisted over a period of 6.5 months. A second event has now been in progress for some eight months. These ions appear to originate at the TS. At V2, 17 AU behind V1, there are a series of 8 increases of low energy ions that occur approximately every 140 days starting in late 2000. Many of these increases can be related to specific periods of high solar activity that occurred some 6 months earlier.",
"doi": "10.1063/1.1809511",
"isbn": "0-7354-0199-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2004-09-15",
"pages": "139-149"
},
{
"id": "authors:b774t-yeg31",
"collection": "authors",
"collection_id": "b774t-yeg31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140319-135713728",
"type": "article",
"title": "Do Anomalous Cosmic Rays Modify the Termination Shock?",
"author": [
{
"family_name": "Florinski",
"given_name": "V.",
"orcid": "0000-0001-5485-2872",
"clpid": "Florinski-V"
},
{
"family_name": "Zank",
"given_name": "G. P.",
"orcid": "0000-0002-4642-6192",
"clpid": "Zank-G-P"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"abstract": "This work extends our previous two-dimensional self-consistent model of the cosmic rays interacting with the solar wind to include anomalous cosmic rays. As before, energetic particles are described kinetically using a Parker equation. The model includes diffusion, convection, and drift effects, as well as shock and compression acceleration and expansion cooling by nonuniform solar wind flow. A new numerical model has been developed featuring an adaptive-mesh refinement algorithm to accommodate small diffusive length scales of low-energy shock-accelerated particles. We show that anomalous cosmic rays have only a minor effect on the termination shock during the time near solar minima. Specifically, cosmic-ray gradients cause the subshock to move away from the Sun by about 1 AU with its compression ratio decreasing by about 5% compared to the reference case without cosmic-ray effects. We also study the effect of solar wind slowdown by charge exchange downstream of the termination shock, producing compressive flow in this region and resulting in additional acceleration of anomalous cosmic rays in the heliosheath. For the first time, spectra calculated with our self-consistent model show a good agreement with the cosmic-ray data from the two Voyager spacecraft, giving more confidence in the model predictions than the previous parametric studies.",
"doi": "10.1086/421901",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2004-08-01",
"series_number": "2",
"volume": "610",
"issue": "2",
"pages": "1169-1181"
},
{
"id": "authors:w96r6-sa675",
"collection": "authors",
"collection_id": "w96r6-sa675",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-084638532",
"type": "article",
"title": "Enhancements of energetic particles near the heliospheric termination shock",
"author": [
{
"family_name": "McDonald",
"given_name": "Frank B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "Bryant C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "Nand",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "William R.",
"clpid": "Webber-W-R"
}
],
"abstract": "The spacecraft Voyager 1 is at a distance greater than 85 au from the Sun, in the vicinity of the termination shock that marks the abrupt slowing of the supersonic solar wind and the beginning of the extended and unexplored distant heliosphere. This shock is expected to accelerate 'anomalous cosmic rays', as well as to re-accelerate Galactic cosmic rays and low-energy particles from the inner Solar System. Here we report a significant increase in the numbers of energetic ions and electrons that persisted for seven months beginning in mid-2002. This increase differs from any previously observed in that there was a simultaneous increase in Galactic cosmic ray ions and electrons, anomalous cosmic rays and low-energy ions. The low-intensity level and spectral energy distribution of the anomalous cosmic rays, however, indicates that Voyager 1 still has not reached the termination shock. Rather, the observed increase is an expected precursor event. We argue that the radial anisotropy of the cosmic rays is expected to be small in the foreshock region, as is observed.",
"doi": "10.1038/nature02066",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2003-11-06",
"series_number": "6962",
"volume": "426",
"issue": "6962",
"pages": "48-51"
},
{
"id": "authors:9x7yk-fme62",
"collection": "authors",
"collection_id": "9x7yk-fme62",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111010-143811077",
"type": "book_section",
"title": "The Coronal Isotopic Composition as Determined Using Solar Energetic Particles",
"book_title": "Solar Wind Ten",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Velli",
"given_name": "Marco",
"clpid": "Velli-M"
},
{
"family_name": "Bruno",
"given_name": "Roberto",
"clpid": "Bruno-R"
},
{
"family_name": "Malara",
"given_name": "Francesco",
"clpid": "Malara-F"
}
],
"abstract": "Solar energetic particles (SEPs), like the solar wind, provide a direct sample of the Sun. Although SEP abundances show a variable amount of mass fractionation, it is possible to develop methods of correcting for it in order to deduce the composition of the corona. Using high-resolution measurements from the Solar Isotope Spectrometer on the Advanced Composition Explorer, we have studied the isotopic composition of 10 abundant elements from C to Ni in 32 large SEP events from late 1997 to the end of 2001 at energies >15 MeV/nucleon. We show that various isotopic and elemental enhancements are correlated with each other, discuss the first order corrections used to account for the variability, and obtain estimated coronal abundances. We compare the coronal values and their uncertainties inferred from SEPs with those that are available from solar wind and meteoritic measurements and find generally good agreement. We include C and Ni isotopic abundances, for which no solar wind measurements have yet been reported.",
"doi": "10.1063/1.1618670",
"isbn": "0-7354-0148-9",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2003-09-02",
"pages": "616-619"
},
{
"id": "authors:rv79x-v6c12",
"collection": "authors",
"collection_id": "rv79x-v6c12",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111028-100805937",
"type": "book_section",
"title": "How Common is Energetic ^3He in the Inner Heliosphere?",
"book_title": "Solar Wind Ten",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Gold",
"given_name": "R. E.",
"clpid": "Gold-R-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Velli",
"given_name": "M.",
"clpid": "Velli-M"
},
{
"family_name": "Bruno",
"given_name": "R.",
"clpid": "Bruno-R"
},
{
"family_name": "Malara",
"given_name": "F.",
"clpid": "Malara-F"
}
],
"abstract": "Using data from the SIS and ULEIS instruments on the Advanced Composition Explorer (ACE) we have identified\nperiods during which energetic ^3He is present in near-Earth interplanetary space between November 1997 and May 2002. The data, which cover the energy intervals 0.2\u20131 MeV/nuc (ULEIS) and 4.5\u201316.3 MeV/nuc (SIS), show that ^3He is present a significant fraction of the time, as would be required if these suprathermal particles were the major source of the ^3He being accelerated by shocks in the interplanetary medium. Specifically, we find that energetic ^3He is present at least ~ 60% of the time, and perhaps significantly more often.",
"doi": "10.1063/1.1618679",
"isbn": "0-7354-0148-9",
"publisher": "American Institute of Physics",
"place_of_publication": "Washington, D.C.",
"publication_date": "2003-09-02",
"pages": "652-655"
},
{
"id": "authors:whjpk-25631",
"collection": "authors",
"collection_id": "whjpk-25631",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-091516862",
"type": "article",
"title": "Elemental Fractionation in Small Solar Energetic Particle Events",
"author": [
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Desai",
"given_name": "M. I.",
"orcid": "0000-0002-7318-6008",
"clpid": "Desai-M-I"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "Using the Solar Isotope Spectrometer on the Advanced Composition Explorer (ACE), we have measured the 11.0-21.8 MeV nucleon^(-1) heavy (Z \u2265 6) element abundances of 39 small solar energetic particle (SEP) events that occurred between 1998 April 3 and 2002 February 26. Using He isotope data from the Ultra-Low-Energy Isotope Spectrometer on ACE, we have classified the events according to their 0.5-2.0 MeV nucleon^(-1) ^3He/^4He ratios. We find that their average heavy-element composition is similar to that of either large gradual events or ^3He-rich events, depending on their ^3He/^4He ratio. As seen in recent studies of small SEP events, we find that the heavy-element intensities relative to C increase with the ^3He/^4He ratios. The dependence of the heavy-element abundances on first ionization potential (FIP) has been derived, using a model consisting of a power law in Q/M (and Z) times a step function in FIP. We report the magnitude of the FIP factor in each event and find that it varies from ~2 to 7 with no clear dependence on the ^3He/^4He ratio.",
"doi": "10.1086/376755",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2003-09-01",
"series_number": "1",
"volume": "594",
"issue": "1",
"pages": "592-604"
},
{
"id": "authors:c0tt0-3fd60",
"collection": "authors",
"collection_id": "c0tt0-3fd60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-164919486",
"type": "article",
"title": "Cosmic ray energy loss in the heliosphere: Direct evidence from electron-capture-decay secondary isotopes",
"author": [
{
"family_name": "Niebur",
"given_name": "S. M.",
"clpid": "Niebur-S-M"
},
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"abstract": "Measurements by the Cosmic Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer (ACE) spacecraft provide direct evidence that galactic cosmic rays lose energy as a result of their interactions with magnetic fields expanding with the solar wind. The secondary isotopes ^(49)V and ^(51)Cr can decay to ^(49)Ti and ^(51)V, respectively, only by electron capture. The observed abundances of these isotopes are directly related to the probability of attaching an electron from the interstellar medium; this probability decreases strongly with increasing energy around a few hundred MeV/nucleon. At the highest energies observed by CRIS, electron attachment on these nuclides is very unlikely, and thus ^(49)V and ^(51)Cr are essentially stable. At lower energies, attachment and decay do occur. Comparison of the energy dependence of the daughter/parent ratios ^(49)Ti/^(49)V and ^(51)V/^(51)Cr during solar minimum and solar maximum conditions confirms that increased energy loss occurs during solar maximum. This analysis indicates an increase in the modulation parameter \u03d5 of about 400 to 700 MV corresponding to an increase in average energy loss for these elements of about 200 to 300 MeV/nucleon.",
"doi": "10.1029/2003JA009876",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2003-08-19",
"series_number": "A10",
"volume": "108",
"issue": "A10",
"pages": "Art. No. 8033"
},
{
"id": "authors:bs6ag-v7g14",
"collection": "authors",
"collection_id": "bs6ag-v7g14",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150403-085521517",
"type": "book_section",
"title": "Voyager Observations of Anomalous Cosmic Ray Gradients and the Role of Diffusion and Drifts in the Outer Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "We find that the diffusion mean free path at 1.5 GV inferred from the gradient of anomalous cosmic rays (ACRs) observed by Voyager 1 and 2 (V1 and V2) has an approximately linear radial distance dependence at solar maximum. At solar minimum the mean free path is a factor of 10 or more larger than at solar maximum. We find that the expected dependence on current sheet tilt of the ACR O V1/V2 gradient has not become evident as of early 2003, likely because the tilt has yet to decrease below \u02dc40\u00b0 . It appears that from mid-2000 up to day 104 of 2003 diffusion is the dominant particle transport mechanism in the far outer heliosphere at 1.5 GV.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:vecmb-ccg63",
"collection": "authors",
"collection_id": "vecmb-ccg63",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150406-141916278",
"type": "book_section",
"title": "Direct Evidence of Energy-Loss in Electron-Capture-Decay Secondary Isotopes in the Heliosphere",
"author": [
{
"family_name": "Scott",
"given_name": "L. M.",
"clpid": "Scott-L-M"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Niebur",
"given_name": "S. M.",
"clpid": "Niebur-S-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "We report direct evidence of the energy loss of galactic cosmic rays as they diffuse in magnetic irregularities expanding with the solar wind. Using the Cosmic\nRay Isotope Spectrometer (CRIS) on the Advanced Composition Explorer (ACE), we report on the energy-dependence of the electron-capture decay of the secondary isotopes ^(49)V and ^(51)Cr. At the highest energies observed by CRIS, where\nelectron attachment is unlikely, ^(49)V and ^(51)Cr are essentially stable; at lower energies the timescale for electron attachment is much shorter and substantial decay\ndoes occur. Comparing the energy dependence of the daughter/parent ratios ^(49)Ti/^(49)V and ^(51)V/^(51)Cr during periods of solar minimum and maximum demonstrates that the solar modulation parameter \u03c6 is about 400 to 700 MV higher\nduring solar maximum than at minimum. Absolute values of \u03c6 inferred from these electron-capture-isotope data agree well with values inferred from comparison of the observed elemental energy spectra with model calculations.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:yhgww-srg24",
"collection": "authors",
"collection_id": "yhgww-srg24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150401-085647968",
"type": "book_section",
"title": "The Solar Cycle Variability of Solar Energetic Particle\n Composition",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-Takaaki"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-Misao"
}
],
"abstract": "Solar particle isotopic composition varies greatly from event to event, apparently due to mass fractionation during particle acceleration and/or transport. We examine whether the amount of this variability changes during the solar cycle and find a strong indication of less isotopic compositional variability at solar maximum than during less active phases. There also seems to be a similar but weaker\nassociation using elemental abundances. The underlying cause of the variability and reasons why it might change over the solar cycle are yet to be determined.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:xv997-g7917",
"collection": "authors",
"collection_id": "xv997-g7917",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150406-132624126",
"type": "book_section",
"title": "The Unusual Solar Particle Events of August 2002",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-Takaaki"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-Misao"
}
],
"abstract": "Several highly unusual solar particle events occurred in August 2002, with high ^3^He/^4He ratios and enormous enhancements of heavy isotopes [5]. By examining\nproton, electron, and heavy ion intensities, H\u03b1, X-ray, and radio flares and particle arrival times relative to them and to coronal mass ejections, we find that the 20 August 2002 event was the largest impulsive event yet seen in this solar cycle at energies >10 MeV/nucleon.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:byhnf-7eb73",
"collection": "authors",
"collection_id": "byhnf-7eb73",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150406-133653562",
"type": "book_section",
"title": "Refractory Nuclides in the Cosmic-Ray Source",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Israel",
"given_name": "M. S.",
"clpid": "Israel-M-S"
},
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "New observations of the abundances and energy spectra of the isotopes of\nMg, Al, and Si from ACE/CRIS are used to extend our previous results on the\ncomposition of refractory nuclides in cosmic-ray source material. For the 18 nuclides\nconsidered for elements between Mg and Ni, relative source abundances are\ngenerally consistent with solar-system values to within 20%. The ^(58)Fe abundance,\ntaken relative to ^(28)Si, is found to have the largest difference from solar, a factor\nof \u223c 1.6. We suggest that the compositional similarity between the cosmic-ray\nsource and the solar system can be understood in terms of acceleration of cosmicray\nrefractories out of a well-mixed sample of interstellar matter.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:as1zh-myv72",
"collection": "authors",
"collection_id": "as1zh-myv72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150403-082902784",
"type": "book_section",
"title": "Heliospheric Termination Shock Mediation by Anomalous Cosmic Rays: Insights from Recent Voyager Data",
"author": [
{
"family_name": "Florinski",
"given_name": "V.",
"orcid": "0000-0001-5485-2872",
"clpid": "Florinski-V"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Zank",
"given_name": "G. P.",
"orcid": "0000-0002-4642-6192",
"clpid": "Zank-G-P"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "The two Voyager spacecraft provide valuable information about the energetic\nparticle population near the termination shock (TS), such as the anomalous\ncosmic ray (ACR) spectra, the intensity gradients, and the radial diffusion coefficients\nobtained from anisotropy measurements. While the spectra and gradients have been modeled successfully using the test-particle approach, the shock modification by the ACR pressure gradient has not yet been addressed in the full\ncontext of the available data. Here we present the results of a self-consistent axisymmetric model of the solar wind modified by both charge exchange and ACR pressure gradients. Our results indicate that during solar minima anomalous cosmic rays with energies above 100 keV are not likely to have a significant impact on the properties of the termination shock.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:5cpnd-ahj08",
"collection": "authors",
"collection_id": "5cpnd-ahj08",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150306-112354854",
"type": "book_section",
"title": "The Approach of Voyager 1 to the Termination Shock",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "T.",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "From 2001 to 2002 the anomalous cosmic ray (ACR) He intensity at 52\nMeV/nuc increased by a factor of \u223c2.2 at Voyager 1. The increase was larger\nat lower energies, indicating that Voyager 1 was 7.5\u00b12.2 AU closer to the termination\nshock in 2002. Since Voyager 1 moved outward 3.8 AU during this time,\nit appears the shock moved inward 3.7\u00b12.2 AU following short term transient\nmotions outward during solar maximum.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:9taz6-5ee10",
"collection": "authors",
"collection_id": "9taz6-5ee10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-090049799",
"type": "article",
"title": "Variability of spectra in large solar energetic particle events",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "Using data from the Solar Isotope Spectrometer on the Advanced Composition Explorer obtained during 36large solar energetic particle events (SEPs) that occurred during 1997\u20132002 we have examined the spectral characteristics of oxygen and iron. Based on the shape of the oxygen spectrum during the decay phase following the peak in particle intensity, each SEP event was categorized as either exponential (7 events) or power law (29 events). We find that the exponential events were typically the larger events (in terms of peak oxygen intensity) and had Fe/O ratios that strongly decreased with increasing energy. Event-averaged Fe/O ratios (integrated over 12 to 60 MeV/nucleon) were at or below coronal abundances for nearly all these events, while the ratios obtained in the power law events were typically enhanced over coronal values. The majority of the power law events had the same spectral index for both O and Fe resulting in an Fe/O ratio independent of energy. However 6 of the 29 power law events had Fe/O ratios that increased with increasing energy due to an Fe spectral index less negative than that of O. We consider simple diffusion theory in an effort to understand the nature of these events and obtain preliminary but promising results.",
"doi": "10.1016/S0273-1177(03)00901-3",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "2003",
"series_number": "12",
"volume": "32",
"issue": "12",
"pages": "2649-2654"
},
{
"id": "authors:vztbp-fqe12",
"collection": "authors",
"collection_id": "vztbp-fqe12",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150306-111608994",
"type": "book_section",
"title": "Unusual Enhancements of MeV Ions and Electrons as Voyager 1 Approaches the Heliospheric Termination Shock",
"author": [
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Heikkila",
"given_name": "B.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "T.",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "In mid-2002 as Voyager 1 moved beyond 85 AU there began an unusual increase of 2.5 MeV ions that remained at a level near 0.1 protons/cm^2-s-sr-MeV for some 6 months. Simultaneously there was an increase in the 2.5 - 70 MeV\nelectrons and in the galactic and anomalous cosmic ray intensity. The electrons are most probably of galactic origin and like the cosmic ray ions are responding to\nthe more favorable modulation levels in the distant heliosphere. It is proposed that the MeV ions are of solar/interplanetary (S/IP) origin with possibly a significant component of IP accelerated pickup ions that have been reaccelerated. Several possibilities for this reacceleration are discussed including the proximity of the\ntermination shock (T.S.).",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:qa19z-t0w96",
"collection": "authors",
"collection_id": "qa19z-t0w96",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150406-135715114",
"type": "book_section",
"title": "New Measurement of the Li, Be, an B Isotopes as a Test of Cosmic Ray Transport Models",
"author": [
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "Precise measurements of predominantly secondary cosmic-ray Li, Be, and B together with current well-measured production cross-sections for these isotopes help to\nimprove our understanding of galactic cosmic ray propagation models. The Cosmic Ray Isotope Spectrometer (CRIS) on ACE has been measuring isotopic composition of cosmic rays since 1997 with high statistical precision. We present the isotopic abundances from CRIS and discuss these observations in the context of cosmic-ray transport models\nand previous cosmic-ray measurements.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:9jmc6-pnc15",
"collection": "authors",
"collection_id": "9jmc6-pnc15",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150306-115444610",
"type": "book_section",
"title": "Voyager 1 Observations of the Anisotropies of Enhanced MeV Ion Fluxes at 85 AU",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Ness",
"given_name": "N. F.",
"clpid": "Ness-N-F"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "T.",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "We report on the diffusive flow anisotropies observed in low-energy protons during intensity increases at Voyager 1 in 2001 and 2002. We propose that the unusual increased intensities after mid-2002 are due to particles accelerated by the solar wind termination shock or by the turbulent interface between the high-speed and low-speed solar wind flows.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:2yegx-d5e02",
"collection": "authors",
"collection_id": "2yegx-d5e02",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150406-143812415",
"type": "book_section",
"title": "Extended Energy Spectrum Measurement of Elements With the Cosmic Ray Isotope Spectrometer (CRIS)",
"author": [
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "We describe a multiple dE/dx technique used to identify particles that penetrate through the bottom of the CRIS instrument, significantly extending the measured energy ranges for major elements beyond that for stopping particles. In preliminary analysis, the upper energy limit for oxygen has been extended from \u223c240 MeV/nuc for stopping particles to \u223c410 MeV/nuc for penetrating particles, and the upper energy limit for iron has been extended from \u223c470 MeV/nuc to \u223c670 MeV/nuc. We report new element intensities in these extended energy ranges, and compare them with previously reported intensities and with spectra derived using cosmic ray transport and solar modulation models.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:14ep6-q9c68",
"collection": "authors",
"collection_id": "14ep6-q9c68",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150305-150054215",
"type": "book_section",
"title": "The ^3He-Rich SEP Events of August 2002: Exceptional Elemental and Isotopic Composition Patterns at Energies Above 10 MeV / Nucleon",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "T.",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-Misao"
}
],
"abstract": "Heavy-ion composition observations from the Solar Isotope Spectrometer on ACE are reported for four ^3He-rich solar-energetic-particle (SEP) events that occurred in August 2002. The abundance enhancement patterns are not monotonic\nfunctions of atomic number (or mass), such as is commonly found in 3He-rich events, but have large enhancements of abundance ratios between some neighboring elements (e.g., N/O) and between isotopes of some elements (e.g., 26Mg/24Mg). The possibility that these patterns could be indicative resonant acceleration of particles within a narrow range of charge-to-mass ratios is considered.",
"publisher": "Universal Academy Press",
"publication_date": "2003"
},
{
"id": "authors:m4s05-nem50",
"collection": "authors",
"collection_id": "m4s05-nem50",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150403-083725157",
"type": "book_section",
"title": "Local Reacceleration of Galactic Cosmic Rays at the Heliosphere's Termination Shock",
"author": [
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Kota",
"given_name": "J.",
"clpid": "Kota-J"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Kajita",
"given_name": "Takaaki",
"clpid": "Kajita-T"
},
{
"family_name": "Asaoka",
"given_name": "Y.",
"clpid": "Asaoka-Y"
},
{
"family_name": "Kawachi",
"given_name": "A.",
"clpid": "Kawachi-A"
},
{
"family_name": "Matsubara",
"given_name": "Y.",
"clpid": "Matsubara-Y"
},
{
"family_name": "Sasaki",
"given_name": "M.",
"clpid": "Sasaki-M"
}
],
"abstract": "The measured intensities in the ecliptic plane of the GCR He (265 MeV/n) and ACR Oxygen (7 - 17 MeV/n) at 70 AU over the solar minimum (1996-1998) of cycle 22 are significantly less than that observed over the 1987 solar minimum of\ncycle 21 at 42 AU. The GCR He at 42 AU is 36% greater than that at 70 AU while ACR O is 5x greater. The different intensity levels and their very different time histories in the opposite phases of the heliomagnetic cycle represent a challenge to modulation theory and must in part be a drift related effect.\n\nKota and Jokipii [1] have modelled the transport of GCRs and ACRs in a 1D model that includes a termination shock and a heliosheath region and in a 2D heliosphere that includes not only drifts but also the effects of an extended\nheliosheath region. They find that near the plane of the ecliptic in qA<0 cycles there is a significant enhancement of GCRs produced by local reacceleration in the heliosheath. This is accompanied by a much larger increase in the ACR O intensity, consistent with the Pioneer/Voyager observations.",
"publisher": "International Union of Applied Physics",
"publication_date": "2003"
},
{
"id": "authors:wwa1c-x2d25",
"collection": "authors",
"collection_id": "wwa1c-x2d25",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150304-160334774",
"type": "article",
"title": "Erratum: Composition of Anomalous Cosmic Rays and Other Heliospheric Ions",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Steenberg",
"given_name": "C. D.",
"clpid": "Steenberg-C-D"
}
],
"doi": "10.1086/345507",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2002-12-20",
"series_number": "2",
"volume": "581",
"issue": "2",
"pages": "1413-1413"
},
{
"id": "authors:qtnkm-r3t34",
"collection": "authors",
"collection_id": "qtnkm-r3t34",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140226-144958207",
"type": "article",
"title": "Composition of Anomalous Cosmic Rays and Other Heliospheric Ions",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Steenberg",
"given_name": "C. D.",
"clpid": "Steenberg-C-D"
}
],
"abstract": "Interstellar pickup ions accelerated by the termination shock of the solar wind dominate the anomalous cosmic-ray (ACR) intensities observed by the Voyager spacecraft in the outer heliosphere. Using a two-dimensional acceleration and propagation model, we derive the relative abundances of these interstellar ACRs and determine the mass dependence of the injection/acceleration efficiency for the diffusive acceleration of H^+, He^+, N^+, O^+, and Ne^+. The energy spectra of C, Na, Mg, Si, S, and Ar also exhibit ACR increases at low energies. To interpret these observations, we have developed a new set of ionization rates for 11 neutral atoms, H, He, C, N, O, Ne, Na, Mg, Si, S, and Ar at 1 AU, and a new set of filtration factors relating neutral densities in the local interstellar medium to those at the location of the solar wind termination shock. Using the injection/acceleration efficiencies and the Ar filtration factor, we estimate the density of neutral Ar to be (3.5 \u00b1 1.6) \u00d7 10^(-7) cm^(-3) in the local interstellar medium. ACR C may have a significant contribution from interstellar neutral C, but the observed intensities of ACR Na, Mg, Si, and S significantly exceed that expected from interstellar neutrals, providing evidence of another source of pickup ions. One possibility discussed is the recently discovered \"inner source\" of singly charged ions that is thought to be solar wind atoms desorbed from interplanetary dust grains.",
"doi": "10.1086/342427",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2002-10-10",
"series_number": "1",
"volume": "578",
"issue": "1",
"pages": "194-210"
},
{
"id": "authors:nemk2-dq215",
"collection": "authors",
"collection_id": "nemk2-dq215",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-085036707",
"type": "article",
"title": "Spectral Properties of He and Heavy Ions in ^3He-rich Solar Flares",
"author": [
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Miller",
"given_name": "J. A.",
"clpid": "Miller-J-A"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Gold",
"given_name": "R. E.",
"clpid": "Gold-R-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Using advanced instrumentation on the ACE spacecraft, we have conducted a survey of solar energetic particle spectra in ^3He-rich events over a broad energy range ~80 keV nucleon^(-1) to 15 MeV nucleon^(-1) during the period 1997 September-2001 March. The spectra of ^4He and heavy ions (C, N, O, Ne, Mg, Si, S, Ca, Fe) were generally similar over this range but often hardened below ~1 MeV nucleon^(-1). In most of the events there was even stronger hardening of the ^3He spectrum below ~1 MeV nucleon^(-1), leading to an energy-dependent ^3He : ^4He ratio. These observations point to unique and distinct properties of ^3He in these events and place new constraints on models that seek to explain enhancements of ^3He and heavy ions using the same mechanisms. In addition to the events with spectra in the form of power laws or double power laws, there is a second class of event in which the low-energy ^3He and Fe spectra are rounded, while the ^4He remains a power law. In these cases ^3He and Fe spectra can be fitted at low energies by a stochastic acceleration model, but this model does not explain the higher energy portions of these spectra, nor the power-law spectral forms of the ^4He. These observations appear to require an additional mechanism, such as acceleration by cascading MHD turbulence. The ^3He enrichment pattern that we observe suggests that all these different spectral features might be due to processes with a common origin but then followed by different acceleration histories.",
"doi": "10.1086/341112",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2002-08-01",
"series_number": "2",
"volume": "574",
"issue": "2",
"pages": "1039-1058"
},
{
"id": "authors:5rmp2-jr938",
"collection": "authors",
"collection_id": "5rmp2-jr938",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-104958666",
"type": "book_section",
"title": "Location of the Termination Shock at Solar Maximum",
"book_title": "Solar Wind Ten Proceedings",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"contributor": [
{
"family_name": "Velli",
"given_name": "M.",
"clpid": "Velli-M"
},
{
"family_name": "Bruno",
"given_name": "R.",
"clpid": "Bruno-R"
},
{
"family_name": "Malara",
"given_name": "F.",
"clpid": "Malara-F"
}
],
"abstract": "During the recent solar maximum, Voyager 1 was beyond 80 AU. Extrapolation of the small gradients of anomalous cosmic rays at solar minimum and the larger gradients at solar maximum indicate that the solar wind termination shock is at \u2272 92 AU at the beginning of 2002.",
"doi": "10.1063/1.1618538",
"isbn": "0-7354-0148-9",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2002-06",
"pages": "47-50"
},
{
"id": "authors:8xpt8-xbe36",
"collection": "authors",
"collection_id": "8xpt8-xbe36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-134134744",
"type": "article",
"title": "Energetic particle composition at 1 au during periods of moderate interplanetary particle fluxes",
"author": [
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "It has recently been proposed that residual energetic ions from preceding impulsive solar energetic particle (SEP) events may contribute to the source population for the larger gradual events accelerated by CME-driven shocks (Mason et al., 1999). This suggests that there may be impulsive SEP material left in interplanetary space during periods relatively free of energetic particle activity. To test this idea we have studied the heavy ions and ^3He present at L1 during periods of low\u2014to\u2014moderate energetic particle fluxes between February 1998 and April 2000. Using the Solar Isotope Spectrometer on the Advanced Composition Explorer, we have measured the energy spectra of heavy elements (Z\u22656) and ^3He over the ranges \u223c8\u201320 MeV/nucleon and \u223c4\u201315 MeV/nucleon, respectively. In these energy spectra, we have looked for spectral and compositional signatures typically characteristic of impulsive or gradual SEP events. We discuss the implications of these observations for the origin of particles accelerated in gradual SEP events.",
"doi": "10.1016/S0273-1177(02)00264-8",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "2002",
"series_number": "1",
"volume": "30",
"issue": "1",
"pages": "97-104"
},
{
"id": "authors:817w6-4ew86",
"collection": "authors",
"collection_id": "817w6-4ew86",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-110121697",
"type": "article",
"title": "Fractionation of solar energetic particles and solar wind according to first ionization potential",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "Although it is well known that solar energetic particles are depleted in elements with first ionization potential (FIP) greater than \u223c10 eV, it is less well known that the degree of FIP fractionation varies from event to event. Similar fractionation patterns and variations are observed in the solar wind, suggesting that these variations may have a common origin. We review evidence for the FIP-related fractionation of SEPs and compare it with FIP fractionation effects in the solar wind at 1 AU. On the basis of several significant differences between the solar wind and SEP compositions, we suggest that most solar energetic particles are not simply an accelerated sample of the average solar wind as observed at 1 AU; rather, solar particles and fast and slow solar wind appear to be distinct samples of coronal material with distinctly different FIP-fractionation patterns.",
"doi": "10.1016/S0273-1177(02)00263-6",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "2002",
"series_number": "1",
"volume": "30",
"issue": "1",
"pages": "79-84"
},
{
"id": "authors:85bh6-bkx41",
"collection": "authors",
"collection_id": "85bh6-bkx41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-082013151",
"type": "article",
"title": "Measurement of the Secondary Radionuclides ^(10)Be, ^(26)Al, ^(36)Cl, ^(54)Mn, and ^(14)C and Implications for the Galactic Cosmic-Ray Age",
"author": [
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
}
],
"abstract": "We report on abundance measurements of ^(10)Be, ^(26)Al, ^(36)Cl, and ^(54)Mn in the Galactic cosmic rays (GCRs) using the Cosmic-Ray Isotope Spectrometer (CRIS) instrument aboard the Advanced Composition Explorer spacecraft at energies from ~70 to ~400 MeV nucleon^(-1). We also report an upper limit on the abundance of GCR ^(14)C. The high statistical significance of these measurements allows the energy dependence of their relative abundances to be studied. A steady-state, leaky-box propagation model, incorporating observations of the local interstellar medium (ISM) composition and density and recent partial fragmentation cross section measurements, is used to interpret these abundances. Using this model, the individual galactic confinement times derived using data for each species are consistent with a unique confinement time value of \u03c4_(esc) = 15.0 \u00b1 1.6 Myr. The CRIS abundance measurements are consistent with propagation through an average ISM hydrogen number density n_H = 0.34 \u00b1 0.04 H atoms cm^(-3). The surviving fractions, f, for each radioactive species have been calculated. From predictions of the diffusion models of Ptuskin & Soutoul, the values of f indicate an interstellar cosmic-ray diffusion coefficient of D = (3.5 \u00b1 2.0) \u00d7 10^(28) cm^2 s^(-1).",
"doi": "10.1086/323842",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2001-12-20",
"series_number": "2",
"volume": "563",
"issue": "2",
"pages": "768-792"
},
{
"id": "authors:0crfh-4w440",
"collection": "authors",
"collection_id": "0crfh-4w440",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-110736601",
"type": "article",
"title": "Solar minimum spectra of galactic cosmic rays and their implications for models of the near-Earth radiation environment",
"author": [
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
}
],
"abstract": "The radiation dose from galactic cosmic rays during a manned mission to Mars is expected to be comparable to the allowable limit for space shuttle astronauts. Most of this dose would be due to galactic cosmic rays with energies < 1 GeV nucleon^(\u22121), with important contributions from heavy nuclei in spite of their low abundance relative to H and He. Using instruments on NASA's Advanced Composition Explorer (ACE) spacecraft, we have made the most statistically precise measurements to date of the solar minimum energy spectra of cosmic ray nuclei with charge Z = 4\u201328 in the energy range \u223c 40\u2013500 MeV nucleon^(\u22121). We compare these measurements obtained during the 1997\u20131998 solar minimum period with measurements from previous solar minima and with models of the near-Earth radiation environment currently used to perform shielding and dose calculations. We find that the cosmic ray heavy-element spectra measured by ACE are as much as 20% higher than previously published solar minimum measurements. We also find significant differences between the ACE measurements and the predictions of available models of the near-Earth radiation environment, suggesting that these models need revision. We describe a cosmic ray interstellar propagation and solar modulation model that provides an improved fit to the ACE measurements compared to radiation environment models currently in use.",
"doi": "10.1029/2000JA000325",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2001-12-01",
"series_number": "A12",
"volume": "106",
"issue": "A12",
"pages": "29979-29987"
},
{
"id": "authors:cpwsd-36m39",
"collection": "authors",
"collection_id": "cpwsd-36m39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111117-145314535",
"type": "book_section",
"title": "The Ionic Charge State Composition at High Energies in\n Large Solar Energetic Particle Events in Solar Cycle 23",
"book_title": "Solar and Galactic Composition",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "The ionic charge states of solar energetic particles (SEPs) depend upon the temperature of the source material and on the environment encountered during acceleration and transport during which electron stripping may occur. Measurements of SEP charge states at relatively high energies (\u227315 MeV/nucleon) are possible with the Mass Spectrometer Telescope (MAST) on the Solar, Anomalous, and Magnetospheric Particle Explorer satellite by using the Earth's magnetic field as a particle rigidity filter. Using MAST data, we have determined ionic charge states of Fe and other elements in several of the largest SEP events of solar cycle 23. The charge states appear to be correlated with elemental abundances, with high charge states (~20 for Fe) for all elements in large Fe-rich events. We review the geomagnetic filter technique and summarize the results from MAST to date, with particular emphasis on new measurements in the very large 14 July 2000 SEP event. We compare the charge states determined by MAST with other measurements and with those expected from equilibrium calculations.",
"doi": "10.1063/1.1433996",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2001-11-21",
"pages": "171-176"
},
{
"id": "authors:cfwe3-neq92",
"collection": "authors",
"collection_id": "cfwe3-neq92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111118-100206530",
"type": "book_section",
"title": "Measurements of the isotopes of lithium, beryllium, and boron from ACE/CRIS",
"book_title": "Solar and Galactic Composition: A Joint SOHO/ACE Workshop",
"author": [
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "The isotopes of lithium, beryllium, and boron (LiBeB) are known in nature to be produced primarily by CNO spallation and \u03b1-\u03b1 fusion from interactions between cosmic rays and interstellar nuclei. While the dominant source of LiBeB isotopes in the present epoch is cosmic-ray interactions, other sources are known to exist, including the production of ^(7)Li from big bang nucleosynthesis. Precise observations of galactic cosmic-ray LiBeB in addition to accurate modeling of cosmic-ray transport can help to constrain the relative importance among the different production mechanisms. The Cosmic Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer (ACE) has measured nuclei with 2 \u2272 Z \u2272 30 in the energy range ~30\u2013500 MeV/nucleon since 1997 with good statistical accuracy. We present measurements of the isotopic abundances of LiBeB and discuss these observations in the context of previous cosmic-ray measurements and spectroscopic observations.",
"doi": "10.1063/1.1434007",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2001-11-21",
"pages": "251-255"
},
{
"id": "authors:f4v4k-a3y91",
"collection": "authors",
"collection_id": "f4v4k-a3y91",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111117-123441068",
"type": "book_section",
"title": "Measurements of Heavy Elements and Isotopes in Small\n Solar Energetic Particle Events",
"book_title": "Solar and Galtic Composition",
"author": [
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "Using the Solar Isotope Spectrometer on the Advanced Composition Explorer, we have examined the ~10\u201320 MeV/nucleon elemental and isotopic composition of heavy (Z\u22656) energetic nuclei accelerated in 30 small solar energetic particle (SEP) events which occurred between 31 March 1998 and 2 January 2001. We have measured the average heavy element content, the ^(22)Ne/^(20)Ne ratio, and the ^(26)Mg/^(24)Mg ratio in these events, and find good agreement with past studies. We have categorized the events according to their 3He/4He ratios, and find significant enhancements in the neutron-rich heavy isotopes of Ne and Mg in the combined 3He-rich data set: ^(22)Ne/^(20)Ne = 0.17\u00b10.05 and ^(26)Mg/^(24)Mg = 0.25\u00b10.05. We discuss the implications of these measurements for the acceleration of energetic nuclei in SEP events.",
"doi": "10.1063/1.1433997",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2001-11-21",
"pages": "177-182"
},
{
"id": "authors:1wjt9-ckz26",
"collection": "authors",
"collection_id": "1wjt9-ckz26",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111118-151333593",
"type": "book_section",
"title": "Constraints on the nucleosynthesis of refractory nuclides in galactic cosmic rays",
"book_title": "Solar and Galactic Composition: A Joint SOHO/ACE Worshop",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "Abundances of the isotopes of the refractory elements Ca, Fe, Co, and Ni in the galactic cosmic-ray source are compared with corresponding abundances in solar-system matter. For the 12 nuclides considered, relative abundances agree to within a factor of 2, and typically within 20\u201330%. In addition, comparisons of cosmic-ray abundances with model calculations of supernova yields are used to argue that cosmic rays contain contributions from stars with a broad range of masses. Based on these and other results we suggest that cosmic rays probably represent a sample of contemporary interstellar matter, at least for refractory species.",
"doi": "10.1063/1.1434010",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2001-11-21",
"pages": "269-274"
},
{
"id": "authors:dwwh0-vtg11",
"collection": "authors",
"collection_id": "dwwh0-vtg11",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111118-134937338",
"type": "book_section",
"title": "Time Variations in Elemental Abundances in Solar Energetic\n Particle Events",
"book_title": "Solar and Galactic Composition",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "St. Cyr",
"given_name": "O. C.",
"orcid": "0000-0001-8906-6097",
"clpid": "St-Cyr-O-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "The Solar Isotope Spectrometer (SIS) on-board the Advanced Composition Explorer has a large collection power and high telemetry rate, making it possible to study elemental abundances in large solar energetic particle (SEP) events as a function of time. Results have now been obtained for more than 25 such events. Understanding the causes of these variations is key to obtaining reliable solar elemental abundances and to understanding solar acceleration processes. Such variations have been previously attributed to two models: (1) a mixture of an initial impulsive phase having enhanced heavy element abundances with a longer gradual phase with coronal abundances and (2) rigidity dependent escape from CME-driven shocks through plasma waves generated by wave-particle interactions. In this second model the injected abundances are assumed to be coronal. Both these models can be expected to depend upon solar longitude since impulsive events are associated with flares at longitudes well-connected magnetically to the observer, and shock properties and connection of the observer to the shock are also longitude dependent. We present results on temporal variations from event to event and within events and show that they appear to have a longitude dependence. We show that the events which have been well-explained by model (2) tend to be near central meridian or the west limb. In addition, we show that there are events with little time variation and heavy element enhancements similar to those of impulsive events. These events seem to be better explained by model (1) with only an impulsive phase.",
"doi": "10.1063/1.1434022",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2001-11-21",
"pages": "343-348"
},
{
"id": "authors:a28wf-j2095",
"collection": "authors",
"collection_id": "a28wf-j2095",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111117-112058199",
"type": "book_section",
"title": "The Phosphorus/Sulfur Abundance Ratio as a Test of Galactic Cosmic-Ray Source Models",
"book_title": "Solar and Galactic Composition",
"author": [
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "Galactic cosmic-ray (GCR) elemental abundances display a fractionation compared to solar-system values that appears ordered by atomic properties such as the first ionization potential (FIP) or condensation temperature (volatility). Determining which parameter controls the observed fractionation is crucial to distinguish between GCR origin models. The Cosmic-Ray Isotope Spectrometer (CRIS) instrument on board NASA's Advanced Composition Explorer (ACE) spacecraft can measure the abundances of several elements that break the general correlation between FIP and volatility (e.g., Na, P, K, Cu, Zn, Ga, and Ge). Phosphorus is a particularly interesting case as it is a refractory (high condensation temperature) element with a FIP value nearly identical to that of its semi-volatile neighbor, sulfur. Using a leaky-box galactic propagation model we find that the P/S and Na/Mg ratios in the GCR source favor volatility as the controlling parameter.",
"doi": "10.1063/1.1434009",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2001-11-21",
"pages": "263-268"
},
{
"id": "authors:4nf5h-9a628",
"collection": "authors",
"collection_id": "4nf5h-9a628",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111118-100325232",
"type": "book_section",
"title": "Long-term fluences of energetic particles in the heliosphere",
"book_title": "Solar and Galactic Composition: A Joint SOHO/ACE Workshop",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Gloeckler",
"given_name": "G.",
"clpid": "Gloeckler-G"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Gold",
"given_name": "R. E.",
"clpid": "Gold-R-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "Robert F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "We report energy spectra of He, O, and Fe nuclei, extending from ~0.3 keV/nucleon to ~300 MeV/nucleon, integrated over the period from the Fall of 1997 to mid-2000. These fluence measurements were made at 1 AU using data from the SWICS, ULEIS, SIS, and CRIS instruments on ACE, and include contributions from fast and slow solar wind, coronal mass ejections, pickup ions, impulsive and gradual solar particle events, acceleration in corotating interaction regions and other interplanetary shocks, and anomalous and galactic cosmic rays. Fluence measurements of six additional species are presented in the energy region from ~0.04 to ~100 MeV/nucleon. We discuss the relative contributions of the various particle components, and comment on the shape and time dependence of the measured energy spectra.",
"doi": "10.1063/1.1433995",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2001-11-21",
"pages": "165-170"
},
{
"id": "authors:xa5bc-4er33",
"collection": "authors",
"collection_id": "xa5bc-4er33",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111116-133416059",
"type": "book_section",
"title": "GCR Neon Isotopic Abundances: Comparison with Wolf-Rayet Star Models and Meteoritic Abundances",
"book_title": "Solar and Galatic Composition",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "Measurements of the neon isotopic abundances from the ACE-CRIS experiment are presented. These abundances have been obtained in seven energy intervals over the energy range of ~80\u2264E\u2264280 MeV/nucleon. The ^(22)Ne/^(20)Ne source ratio is derived using the measured ^(21)Ne/^(20)Ne abundance as a \"tracer\" of secondary production of the neon isotopes. We find that the ^(22)Ne/^(20)Ne abundance ratio at the cosmic-ray source is a factor of 5.0\u00b10.2 greater than in the solar wind. The GCR ^(22)Ne/^(20)Ne ratio is also shown to be considerably larger than that found in anomalous cosmic rays, solar energetic particles, most meteoritic samples of matter, and interplanetary dust particles. Recent two-component Wolf-Rayet models provide predictions for the ^(22)Ne/^(20)Ne ratio and other isotope ratios. Comparison of the CRIS neon, iron, and nickel isotopic source abundance ratios with predictions indicate possible enhanced abundances of some neutron-rich nuclides that are expected to accompany the ^(22)Ne excess.",
"doi": "10.1063/1.1434008",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2001-11-21",
"pages": "257-262"
},
{
"id": "authors:9761w-rtt08",
"collection": "authors",
"collection_id": "9761w-rtt08",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111117-080853257",
"type": "book_section",
"title": "Solar Coronal Abundances of Rare Elements Based on Solar\n Energetic Particles",
"book_title": "Solar and Galactic Composition",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "Although solar energetic particle (SEP) abundances vary from event to event, it has been shown that by accounting for these variations it is possible to use SEP data to obtain reliable estimates of elemental abundances for the solar corona. We analyze ~20 to 65 MeV/nucleon measurements from the Solar Isotope Spectrometer on ACE in large SEP events observed from November 1997 to January 2001 to obtain new values of the average SEP composition of rare species, P, Cl, K, Ti, Mn, Cr, Co, Cu, and Zn, which have had limited statistical accuracy in SEPs in the past. The measured SEP abundances are compared with other sources of solar-system composition data.",
"doi": "10.1063/1.1433987",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2001-11-21",
"pages": "107-112"
},
{
"id": "authors:m8v97-xh028",
"collection": "authors",
"collection_id": "m8v97-xh028",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111118-075529994",
"type": "book_section",
"title": "Galactic Abundances: Report of Working Group 3",
"book_title": "Solar and Galactic Composition",
"author": [
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Bothmer",
"given_name": "V.",
"clpid": "Bothmer-V"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Keller",
"given_name": "J. W.",
"clpid": "Keller-J-W"
},
{
"family_name": "Salerno",
"given_name": "E.",
"clpid": "Salerno-E"
},
{
"family_name": "Sofia",
"given_name": "U. J.",
"clpid": "Sofia-U-J"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Thielemann",
"given_name": "F.-K.",
"clpid": "Theilemann-F-K"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Buclin",
"given_name": "F.",
"clpid": "Buclin-F"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Fl\u00fcckiger",
"given_name": "E. O.",
"clpid": "Fl\u00fcckiger-E-O"
},
{
"family_name": "Hofer",
"given_name": "M. Y.",
"clpid": "Hofer-M-Y"
},
{
"family_name": "Jones",
"given_name": "F. C.",
"clpid": "Jones-F-C"
},
{
"family_name": "Kirilova",
"given_name": "D.",
"clpid": "Kirilova-D"
},
{
"family_name": "Kunow",
"given_name": "H.",
"clpid": "Kunow-H"
},
{
"family_name": "Laming",
"given_name": "M.",
"clpid": "Laming-M"
},
{
"family_name": "Tranquille",
"given_name": "C.",
"clpid": "Tranquille-C"
},
{
"family_name": "Wenzel",
"given_name": "K.-P.",
"clpid": "Wenzel-K-P"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "We summarize the various methods and their limitations and strengths to derive galactic abundances from in-situ and remote-sensing measurements, both from ground-based observations and from instruments in space. Because galactic abundances evolve in time and space it is important to obtain information with a variety of different methods covering different regions from the Very Local Insterstellar Medium (VLISM) to the distant galaxy, and different times throughout the evolution of the galaxy. We discuss the study of the present-day VLISM with neutral gas, pickup ions, and Anomalous Cosmic Rays, the study of the local interstellar medium (ISM) at distances <1.5 kpc utilizing absorption line measurements in H I clouds, and the study of galactic cosmic rays, sampling contemporary (~15 Myr) sources in the local ISM within a few kiloparsec of the solar system. Solar system abundances, derived from solar abundances and meteorite studies are discussed in several other chapters of this volume. They provide samples of matter from the ISM from the time of solar system format ion, about 4.5 Gyr ago. The evolution of galactic abundances on longer time scales is discussed in the context of nuclear synthesis in the various contributing stellar objects.",
"doi": "10.1063/1.1434002",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2001-11-21",
"pages": "207-220"
},
{
"id": "authors:609ya-bb713",
"collection": "authors",
"collection_id": "609ya-bb713",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111118-094513677",
"type": "book_section",
"title": "Isotopic Abundances in the Solar Corona as Inferred from\n ACE Measurements of Solar Energetic Particles",
"book_title": "Solar and Galactic Composition",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "The isotopic composition of solar energetic particles (SEPs) has been measured using the Solar Isotope Spectrometer on the Advanced Composition Explorer. The measurements include up to 12 isotope abundance ratios for ten elements from C through Ni at energies of tens of MeV/nucleon in 18 large SEP events that have occurred since November 1997. These measurements clearly establish that SEP isotopic composition can vary widely (by factors of >3) from event to event, presumably due to mass fractionation processes during particle acceleration and/or transport. Elemental and isotopic abundance ratios are strongly correlated, suggesting that elemental and isotopic fractionation relative to the coronal source are largely governed by the same processes. Using empirical correlations to correct for the fractionation and obtain the coronal isotopic composition yields preliminary abundance values in good agreement with those found in the solar wind, with comparable accuracy.",
"doi": "10.1063/1.1433990",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2001-11-21",
"pages": "127-132"
},
{
"id": "authors:babjv-nnp37",
"collection": "authors",
"collection_id": "babjv-nnp37",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-085913469",
"type": "article",
"title": "Forecasting the arrival of shock-accelerated solar energetic particles at Earth",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Energetic particles accelerated at interplanetary shocks can result in an increased radiation dose for astronauts as well as an increased risk to satellite hardware. These shocks are known to occasionally accelerate protons to energies greater than 100 MeV and can result in very high fluxes. Advanced warning of the arrival of strong interplanetary shocks can enable steps to be taken to minimize the potential risks. In an effort to monitor and assess the radiation risk to astronauts, two real-time count rate monitors were implemented in the Solar Isotope Spectrometer (SIS) on the ACE spacecraft. These rates measure protons with energies >10 and >30 MeV. Since ACE is located at the L1 Lagrangian point, these rates provide information and warning up to 1 hour before an interplanetary shock reaches Earth. Using ACE and GOES, data we have examined examples of shocks and associated energetic particles that have been detected at ACE and were later observed near Earth in an effort to develop more fully the forecasting capability of ACE. Because of the limited amount of solar activity during 1997\u20131999, this current work is primarily a proof of concept.",
"doi": "10.1029/2000JA000216",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "2001-10-01",
"series_number": "A10",
"volume": "106",
"issue": "A10",
"pages": "20979-20983"
},
{
"id": "authors:btrqg-5hc77",
"collection": "authors",
"collection_id": "btrqg-5hc77",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-154628633",
"type": "article",
"title": "Radioactive clocks and cosmic-ray transport in the galaxy",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Niebur",
"given_name": "S. M.",
"clpid": "Niebur-S-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "There are a number of radioactive 'clocks' in the cosmic radiation that can be used to measure the time scales for cosmic ray processes in the Galaxy. With high-resolution isotope measurements available from ACE it is now possible to read these clocks with greatly improved accuracy and address key questions about the origin and lifetime of cosmic rays. This paper discusses the status of three such investigations.",
"doi": "10.1023/A:1013868225842",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2001-10",
"series_number": "1-4",
"volume": "99",
"issue": "1-4",
"pages": "27-39"
},
{
"id": "authors:x4yd0-9e422",
"collection": "authors",
"collection_id": "x4yd0-9e422",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-090214937",
"type": "article",
"title": "The Origin of Primary Cosmic Rays: Constraints from ACE Elemental and Isotopic Composition Observations",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M-L"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Cosmic-ray isotope observations from NASA's Advanced Composition Explorer (ACE) mission have been used to investigate the composition of cosmic-ray source material. Source abundances relative to ^(56)Fe are reported for eleven isotopes of Ca, Fe, Co, and Ni, including the very rare isotopes ^(48)Ca and ^(64)Ni. Although the source abundances range over a factor \u223c10^4, most of the ratios to ^(56)Fe are consistent with solar-system values to within \u223c20%. However, there are some notable differences, the most significant being an excess of \u223c(70\u00b130)% relative to the solar system for the cosmic-ray source ratio ^(58)Fe/^(56)Fe. The possible association of such an excess with a contribution to the cosmic-ray source from Wolf\u2013Rayet star ejecta is discussed.",
"doi": "10.1023/A:1013816209004",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "2001-10",
"series_number": "1-4",
"volume": "99",
"issue": "1-4",
"pages": "15-26"
},
{
"id": "authors:mx45x-aw996",
"collection": "authors",
"collection_id": "mx45x-aw996",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-103636832",
"type": "book_section",
"title": "Isotopic abundances in the solar corona as inferred from ACE measurements of solar energetic particles",
"book_title": "Solar and Galactic Composition",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "R. F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "The isotopic composition of solar energetic particles (SEPs) has been measured using the Solar Isotope Spectrometer on the Advanced Composition Explorer. The measurements include up to 12 isotope abundance ratios for ten elements from C through Ni at energies of tens of MeV/nucleon in 18 large SEP events that have occurred since November 1997. These measurements clearly establish that SEP isotopic composition can vary widely (by factors of >3) from event to event, presumably due to mass fractionation processes during particle acceleration and/or transport. Elemental and isotopic abundance ratios are strongly correlated, suggesting that elemental and isotopic fractionation relative to the coronal source are largely governed by the same processes. Using empirical correlations to correct for the fractionation and obtain the coronal isotopic composition yields preliminary abundance values in good agreement with those found in the solar wind, with comparable accuracy.",
"doi": "10.1063/1.1433990",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2001-03",
"pages": "127-132"
},
{
"id": "authors:jz2fp-rsv41",
"collection": "authors",
"collection_id": "jz2fp-rsv41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111222-093454569",
"type": "book_section",
"title": "The cosmic-ray contribution to galactic abundances of the light elements: Interpretation of GCR LiBeB abundance measurements from ACE/CRIS",
"book_title": "Solar and Galactic Composition",
"author": [
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Wimmer-Schweingruber",
"given_name": "Robert F.",
"clpid": "Wimmer-Schweingruber-R-F"
}
],
"abstract": "Inelastic collisions between the galactic cosmic rays (GCRs) and the interstellar medium (ISM) are responsible for producing essentially all of the light elements Li, Be, and B (LiBeB) observed in the cosmic rays. Previous calculations (e.g., [1]) have shown that GCR fragmentation can explain the bulk of the existing LiBeB abundance in the present day Galaxy. However, elemental abundances of LiBeB in old halo stars indicate inconsistencies with this explanation. We have used a simple leaky-box model to predict the cosmic-ray elemental and isotopic abundances of LiBeB in the present epoch. We conducted a survey of recent scientific literature on fragmentation cross sections and have calculated the amount of uncertainty they introduce into our model. The predicted particle intensities of this model were compared with high energy (E_(ISM) = 200\u2013500\u200aMeV/nucleon) cosmic-ray data from the Cosmic Ray Isotope Spectrometer (CRIS), which indicates fairly good agreement with absolute fluxes for Z \u2265 5 and relative isotopic abundances for all LiBeB species.",
"doi": "10.1063/1.1434006",
"isbn": "0-7354-0042-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2001-03",
"pages": "245-250"
},
{
"id": "authors:vssqq-ryt18",
"collection": "authors",
"collection_id": "vssqq-ryt18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150302-135738779",
"type": "book_section",
"title": "The Heavy Nuclei eXplorer (HNX) Mission",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Adams",
"given_name": "J. H., Jr.",
"clpid": "Adams-J-H-Jr"
},
{
"family_name": "Barbieri",
"given_name": "M.",
"clpid": "Barbieri-M"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Craig",
"given_name": "N.",
"clpid": "Craig-N"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Doke",
"given_name": "T.",
"clpid": "Doke-T"
},
{
"family_name": "Hasebe",
"given_name": "N.",
"clpid": "Hasebe-N"
},
{
"family_name": "Hayashe",
"given_name": "T.",
"clpid": "Hayashe-T"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Lee",
"given_name": "D.",
"clpid": "Lee-D"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mark",
"given_name": "D.",
"clpid": "Mark-D"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mitchell",
"given_name": "J. W.",
"clpid": "Mitchell-J-W"
},
{
"family_name": "Ogura",
"given_name": "K.",
"clpid": "Ogura-K"
},
{
"family_name": "Schindler",
"given_name": "S. M.",
"clpid": "Schindler-S-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Tarle",
"given_name": "G.",
"clpid": "Tarle-G"
},
{
"family_name": "Tawara",
"given_name": "H.",
"clpid": "Tawara-H"
},
{
"family_name": "Waddington",
"given_name": "C. J.",
"clpid": "Waddington-C-J"
},
{
"family_name": "Westphal",
"given_name": "A. J.",
"clpid": "Westphal-A-J"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yasuda",
"given_name": "N.",
"clpid": "Yasuda-N"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "The primary scientific objectives of HNX, which was recently selected by NASA for a Small Explorer (SMEX) Mission Concept Study, are to measure the age of the galactic cosmic rays (GCR) since nucleosynthesis, determine the injection mechanism for the GCR accelerator (Volatility or FIP), and study the mix of nucleosynthetic processes that contribute to the source of GCRs. The experimental goal of HNX is to measure the elemental abundances of all individual stable nuclei from neon through the actinides and possibly beyond. HNX is composed of two instruments: ECCO, which measures elemental abundances of nuclei with Z\u226572, and ENTICE, which measures elemental abundances of nuclei with 10\u2264Z\u226482. We describe the mission and the science that can be addressed by HNX. 1. Introduction The Heavy Nuclei eXplorer (HNX) mission that is currently being studied as a possible Small Explorer Mission (SMEX) has the primary objective of determining the origin of the galactic cosmic rays. The abundance patterns of the elements and isotopes in the GCRs provide the key because they are the fingerprints of GCR origin. HNX will, for the first time, measure with high precision the abundance of every individual element in the periodic table from neon through the actinides (thorium, uranium, plutonium, curium, and perhaps beyond). The HNX spacecraft will carry two high-precision instruments, the Extremely-heavy Cosmic-ray Composition Observer (ECCO) and the ENergetic Trans-Iron Composition Experiment (ENTICE), which cover overlapping ranges of the periodic table (Figure 1).",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:97ex1-m2g09",
"collection": "authors",
"collection_id": "97ex1-m2g09",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150302-110723970",
"type": "book_section",
"title": "Onset of Solar Modulation in the Outer Heliosphere as Seen in Anomalous Cosmic Rays",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "We examine intensities and gradients of anomalous cosmic rays determined from observations on the Voyager 1 and 2 spacecraft to study the rapid increase in solar modulation that begins near mid-2000. We suggest that these effects are due to the arrival in the region of the spacecraft of complex magnetic field topologies associated with the reversal of the Sun's magnetic field.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:atyfe-yze51",
"collection": "authors",
"collection_id": "atyfe-yze51",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-111154005",
"type": "book_section",
"title": "Solar Energetic Particle Anisotropies from the ACE Solar Isotope Spectrometer",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "deNolfo",
"given_name": "G. A.",
"clpid": "deNolfo-G-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "Although not specifically designed for it, the Solar Isotope Spectrometer (SIS) on the Advanced Composition Explorer spacecraft is sensitive to particle anisotropies of heavy ions at energies of tens of MeV/nucleon. Using the arrival time of each particle (to the nearest second) and the trajectory measured with the instrument's position sensing detector, the arrival direction of each particle may be determined to \u02dc30\u00b0 in azimuth about the spacecraft spin axis and to better than 1\u00b0 in zenith angle from the axis. This allows the angular distribution of particles to be measured within the \u02dc145\u00b0 wide field of view of the instrument, from which the intensities both along the field and perpendicular to it can usually be determined. We describe how anisotropies are obtained from SIS and present examples demonstrating some of the capabilities of SIS in studying anisotropies. With further analysis, SIS can contribute to studies exploring the dependence of particle angular distributions on energy and species.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:1rs1t-36b39",
"collection": "authors",
"collection_id": "1rs1t-36b39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-102207197",
"type": "book_section",
"title": "Examining the Abundances of Rare Elements in Solar Energetic Particle Events",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "Using data accumulated with the Solar Isotope Spectrometer on ACE during 27 large solar energetic particle (SEP) events the effects of charge-to-mass (Q/M) fractionation on rare elements are examined. In an attempt to correct for these fractionation effects and obtain preliminary estimates of the coronal abundances of K, Ti, Cr, Mn, Co, Ni, Cu, and Zn, the SEP events are classified according to their Fe/Si ratio. The data from all events within an Fe/Si category are summed and the rare element abundances extracted over an energy interval of 20 to 65 MeV/nucleon. We estimated the apparent Q/M fractionation, corrected for it, and obtained initial results which are encouraging.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:39e8v-n7704",
"collection": "authors",
"collection_id": "39e8v-n7704",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-100220896",
"type": "book_section",
"title": "Temporal Variations in Solar Energetic Particle Events",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "The Solar Isotope Spectrometer (SIS) on-board the Advanced Composition Explorer (ACE) spacecraft has measured elemental abundances in large solar energetic particle\n(SEP) events as a function of time for more than 25\nsuch events. There are large temporal variations in the observed abundances within events, from event to event, and\nas a function of particle energy. Such variations have been\npreviously attributed to the combination of an initial impulsive phase having enhanced heavy element abundances with a longer gradual phase with coronal abundances. More recently they have been attributed to rigidity dependent escape from CME-driven shocks through plasma waves generated\nby wave-particle interactions. Both these models can\nbe expected to depend upon solar longitude since impulsive\nevents are associated with longitudes well-connected magnetically to the observer, and shock properties and connection of the observer to the shock are also longitude dependent. We present evidence of longitude related variations. In addition, we show that there are events with little time variation and heavy element enhancements similar to those of impulsive events. These events appear to be difficult to explain in current models in which particles are accelerated with coronal abundances. Rather, these events seem to require abundance enhancements either in the source material or in the acceleration process.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:rrt4w-xvp29",
"collection": "authors",
"collection_id": "rrt4w-xvp29",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-132540360",
"type": "article",
"title": "Distinguishing galactic cosmic-ray source models with first ionization potential and volatility",
"author": [
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Barghouty",
"given_name": "A. F.",
"clpid": "Barghouty-A-F"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"abstract": "Studies of the galactic cosmic-ray source composition reveal a pattern in the elemental abundances that may be controlled by the first ionization potential (FIP) or a closely correlated parameter, the condensation temperature (volatility). Determining the true parameter is key identifying the galactic cosmic-ray source (GCRS) material. Using data from the CRIS instrument onboard the ACE spacecraft, we examine five elements that are more volatile than other elements of similar FIP. Three of these (Na, Cu, Ge) show small deficits in their source abundances that may suggest a volatility-dependent fractionation. The source abundances of Ga and Zn (an intermediate FIP element) are consistent with either model. Possible systematic uncertainties from the cosmic-ray pathlength estimate as well as effects due to the instrumental acceptance are discussed. We also compare the GCRS composition to that observed in solar energetic particles.",
"doi": "10.1016/S0273-1177(01)00116-8",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "2001",
"series_number": "4",
"volume": "27",
"issue": "4",
"pages": "779-784"
},
{
"id": "authors:bhrzc-wn317",
"collection": "authors",
"collection_id": "bhrzc-wn317",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-110535538",
"type": "book_section",
"title": "Are Solar Energetic Particles an Accelerated Sample of Solar Wind?",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "In the current picture of gradual solar energetic particle (SEP) events, the acceleration is believed to take place at a shock driven by a coronal mass ejection as it moves through the corona and out into the solar wind. It is\noften assumed that the solar wind provides the seed\nparticles that are accelerated and later observed at 1 AU.\nWe compare solar energetic particle and solar wind\ncomposition measurements, focusing on a comparison of\nthe fractionation patterns with respect to first ionization\npotential. On the basis of several significant differences\nbetween the solar wind and SEP compositions, we conclude\nthat most SEPs with energies >5 MeV/nucleon are not\nsimply an accelerated sample of solar wind. Rather, SEPs\nand fast and slow solar wind appear to be distinct samples\nof coronal material with significantly different fractionation patterns. This implies that solar energetic particles must be accelerated within a few solar radii of the Sun.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:80drf-86g62",
"collection": "authors",
"collection_id": "80drf-86g62",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-102937851",
"type": "book_section",
"title": "Mass Fractionation in Solar Energetic Particles and the Isotopic Composition of the Corona",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "Using the Solar Isotope Spectrometer on the Advanced\nComposition Explorer, the isotopic composition of solar energetic particles (SEPs) has been measured in 18\nlarge SEP events for abundant elements from C through Ni\nat energies of tens of Me V /nucleon. Although SEP isotopic\ncomposition is found to vary widely from event to event, it is strongly correlated with the elemental composition, suggesting that elemental and isotopic fractionation relative to the coronal source are largely governed by the same processes. Using empirical correlations to correct for the fractionation yields preliminary coronal isotopic abundance values in good agreement with those found in the solar wind, with comparable accuracy.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:7v9wq-d1223",
"collection": "authors",
"collection_id": "7v9wq-d1223",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-114316464",
"type": "book_section",
"title": "The Evolution of Galactic Cosmic Ray Element Spectra from Solar Minimum to Solar Maximim: ACE Measurements",
"author": [
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "The spectra of galactic cosmic ray (GCR) elements from Beryllium to Nickel in the energy range 40 - 500 MeV/nucleon at 1 AU are being continuously measured by\ninstruments on-board the Advanced Composition Explorer\n(ACE). The collecting power of these instruments allows statistically precise spectra to be calculated every few months for most elements. Measurements of temporal variations in GCR spectra over the solar cycle are important for understanding solar modulation processes, and also for refining models of the near-earth radiation environment used to perform shielding and dose calculations for manned and unmanned space missions. We report on ACE observations of the evolution of GCR element spectra from solar minimum in 1997 through Spring 2001. We find significant differences between the ACE measurements and the predictions of available models of the near-Earth radiation environment, suggesting that these models need revision. We describe a cosmic ray interstellar propagation and solar modulation model that provides an improved fit to the ACE measurements compared to radiation environment models currently in use.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:7m8rw-9bf22",
"collection": "authors",
"collection_id": "7m8rw-9bf22",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-112434005",
"type": "article",
"title": "The isotopic source composition of cosmic-ray iron, cobalt, and nickel",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"abstract": "The isotopic composition of cosmic-ray Fe, Co, and Ni at energies \u223c150\u2013500 MeV/nucleon has been measured with the Cosmic-Ray Isotope Spectrometer (CRIS) instrument on ACE. Source abundances have been derived from a leaky-box propagation model using secondary species in the range 41 \u2264 A \u2264 55 to constrain the calculated secondary contributions to the Fe, Co, and Ni isotopes. The derived relative source abundances bear a strong resemblance to solar-system values. The most significant difference, an excess of \u223c (70 \u00b1 30)%, is found for the source abundance ratio ^(58)Fe/^(56)Fe. Some implications of the derived source composition for the origin of cosmic rays are discussed.",
"doi": "10.1016/S0273-1177(01)00120-X",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "2001",
"series_number": "4",
"volume": "27",
"issue": "4",
"pages": "773-778"
},
{
"id": "authors:dhrxa-zn407",
"collection": "authors",
"collection_id": "dhrxa-zn407",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-113218886",
"type": "book_section",
"title": "Effects of Increasing Solar Modulation on Anomalous Cosmic Ray Intensities",
"author": [
{
"family_name": "Sollitt",
"given_name": "L. S.",
"clpid": "Sollitt-L-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-Manfred"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "Anomalous Cosmic Rays (ACRs) are accelerated far out in the heliosphere at the termination shock. As they diffuse back through the solar system to 1 AU, they are modulated in intensity. The intensity of ACRs at 1 AU observed by the Solar Isotope Spectrometer has been decreasing since September 1997 as solar activity has been increasing. Oxygen at 7.1-10 MeV/nuc has decreased by a factor of at least 80. Nitrogen and neon at similar energies have also had similar large decreases. We examine the changing fluxes of various ACR species, and the changing elemental and isotopic composition of ACRs. ACR oxygen, in particular, may no longer be observable in 2001 at 1 AU above the background of solar, interplanetary, and galactic cosmic ray particles. The 22 Ne/20 Ne ratio at 15 MeV/nuc has also been increasing since September 1997 from a value of about 0.1 to a value more consistent with the GCR ratio of 0.5. This suggests that GCRs now dominate the quiet time flux of Ne at energies of 10 to 30 MeV/nucleon.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:6pgv0-29k72",
"collection": "authors",
"collection_id": "6pgv0-29k72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-105420424",
"type": "book_section",
"title": "Average Elemental and Isotopic Composition of Small Solar Energetic Particle Events",
"author": [
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-Manfred"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "Using the Solar Isotope Spectrometer on the Advanced Composition Explorer, we have measured the heavy (Z\u22656) element abundances of 33 small solar energetic particle (SEP) events which occurred between 4 April, 1998 and 3 December, 2000. The events have been classified according to their elemental and isotopic composition as well as other defining characteristics. With the event-averaged heavy element fluxes, we have investigated the dependence of elemental abundances relative to those of the solar photosphere on first ionization potential (FIP). Where possible, we have examined the FIP fractionation effects on the average composition of the small SEP events, and discuss the ensuing implications for the origin and acceleration of nuclei in these events.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:0y30s-8r716",
"collection": "authors",
"collection_id": "0y30s-8r716",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150305-131051186",
"type": "conference_item",
"title": "Examining the Abundance of Rare Elements in Solar Energetic Particle Events",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "Using data accumulated with the Solar Isotope Spectrometer on ACE during 27 large solar energetic pa1ticle (SEP) events the effects of charge-to-mass (Q/M) fractionation\non rare elements arc examined. In an attempt to correct for these fractionation effects and obtain preliminary\nestimates of the coronal abundances of K, Ti, Cr, Mn, Co, Ni, Cu, and Zn, the SEP events are classified according to their Fe/Si ratio. The data from all events within an Fe/Si category are summed and the rare element abundances extracted over an energy interval of 20 to 65 MeV/nucleon. We estimated the apparent Q/M fractionation, corrected for it, and obtained initial results which are encouraging.",
"publisher": "Caltech Library",
"publication_date": "2001"
},
{
"id": "authors:qxcnn-37f36",
"collection": "authors",
"collection_id": "qxcnn-37f36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200508-135103238",
"type": "book_section",
"title": "Radioactive Clocks and Cosmic-Ray Transport in the Galaxy",
"book_title": "The Astrophysics of Galactic Cosmic Rays",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Niebur",
"given_name": "S. M.",
"clpid": "Niebur-S-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Diehl",
"given_name": "Roland",
"clpid": "Diehl-R"
},
{
"family_name": "Parizot",
"given_name": "Etienne",
"clpid": "Parizot-E"
},
{
"family_name": "Kallenbach",
"given_name": "Reinald",
"clpid": "Kallenbach-R"
},
{
"family_name": "von Steiger",
"given_name": "Rudolf",
"clpid": "von-Steiger-R"
}
],
"abstract": "There are a number of radioactive 'clocks' in the cosmic radiation that can be used to measure the time scales for cosmic ray processes in the Galaxy. With high-resolution isotope measurements available from ACE it is now possible to read these clocks with greatly improved accuracy and address key questions about the origin and lifetime of cosmic rays. This paper discusses the status of three such investigations.",
"doi": "10.1007/978-94-017-3239-0_3",
"isbn": "9789048158621",
"publisher": "Springer Netherlands",
"place_of_publication": "Dordrecht",
"publication_date": "2001",
"pages": "27-39"
},
{
"id": "authors:668ap-x0037",
"collection": "authors",
"collection_id": "668ap-x0037",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-111820409",
"type": "book_section",
"title": "Fluences of Solar, Heliospheric, and Galactic Particles at 1 AU",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Gloeckler",
"given_name": "G.",
"clpid": "Gloeckler-G"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Gold",
"given_name": "R. E.",
"clpid": "Gold-R-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Zurbechen",
"given_name": "T. H.",
"clpid": "Zurbechen-T-H"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "We report energy spectra of He, O, and Fe nuclei from ~0.3 keV/nucleon to ~300 MeV/nucleon, integrated from late-1997 to mid-2000. These fluence measurements were made at 1 AU using data from instruments on ACE, and include contributions from fast and slow solar wind, coronal mass ejections, pickup ions, impulsive and gradual solar particle events, particles accelerated in corotating interaction regions and other interplanetary shocks, and anomalous and galactic cosmic rays. Fluence measurements of six additional species are presented from ~0.04 to ~100 MeV/nucleon. We discuss the relative contributions of various particle components, comment on the energy spectra, and consider the implications for particle acceleration processes, cosmic ray spectra and particles implanted in the lunar soil.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:6ak2k-cdd89",
"collection": "authors",
"collection_id": "6ak2k-cdd89",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150302-133152754",
"type": "book_section",
"title": "The Energetic Trans-Iron Composition Experiment (ENTICE) on the Heavy Nuclei Explorer (HNX) Mission",
"author": [
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Adams",
"given_name": "J. H., Jr.",
"clpid": "Adams-J-H-Jr"
},
{
"family_name": "Barbier",
"given_name": "L. M.",
"clpid": "Barbier-L-M"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Craig",
"given_name": "N.",
"clpid": "Craig-N"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Doke",
"given_name": "T.",
"clpid": "Doke-T"
},
{
"family_name": "Hasebe",
"given_name": "N.",
"clpid": "Hasebe-N"
},
{
"family_name": "Hayashi",
"given_name": "T.",
"clpid": "Hayashi-T"
},
{
"family_name": "Lee",
"given_name": "D.",
"clpid": "Lee-D"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mark",
"given_name": "D.",
"clpid": "Mark-D"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Mitchell",
"given_name": "J. W.",
"clpid": "Mitchell-J-W"
},
{
"family_name": "Ogura",
"given_name": "K.",
"clpid": "Ogura-K"
},
{
"family_name": "Schindler",
"given_name": "S. M.",
"clpid": "Schindler-S-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Tarl",
"given_name": "G.",
"clpid": "Tari-G"
},
{
"family_name": "Tawara",
"given_name": "H.",
"clpid": "Tawara-H"
},
{
"family_name": "Waddington",
"given_name": "C. J.",
"clpid": "Waddington-C-J"
},
{
"family_name": "Westphal",
"given_name": "A .J.",
"clpid": "Westphal-A-J"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yasuda",
"given_name": "N.",
"clpid": "Yasuda-N"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-Manfred"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "The HNX mission is composed of the ENTICE and ECCO experiments. The experimental goal of ENTICE is to measure with high precision the elemental abundances of all nuclei with 10\u2264Z\u226482. This will enable us to determine if the injection mechanism for the cosmic ray accelerator is controlled by FIP or Volatility and to study the mix of nucleosynthetic processes that contribute to the galactic cosmic ray source. The ENTICE experiment utilizes the dE/dx-C method of charge determination and consists of silicon dE/dx detectors, Cherenkov detectors with two different refractive indices, and a fiber hodoscope. We will describe the instrument and its performance based on beam tests of a prototype instrument.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:0x5zr-b1w10",
"collection": "authors",
"collection_id": "0x5zr-b1w10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-133307053",
"type": "article",
"title": "Galactic cosmic ray neon isotopic abundances measured by the cosmic ray isotope spectrometer (CRIS) on ACE",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"abstract": "We present measurements of neon isotopic abundances from the ACE-CRIS experiment. These abundances have been obtained in seven energy intervals over the energy range of \u223c80\u2264E\u2264280 MeV/nucleon. We find that the ^(22)Ne/^(20)Ne abundance ratio at the cosmic-ray source is a factor of 5.0\u00b10.2 greater than for the solar wind. These measured abundances agree well with previous experiments. The significance of these results is discussed.",
"doi": "10.1016/S0273-1177(01)00119-3",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "2001",
"series_number": "4",
"volume": "27",
"issue": "4",
"pages": "767-772"
},
{
"id": "authors:q31da-0pd79",
"collection": "authors",
"collection_id": "q31da-0pd79",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150304-133315782",
"type": "book_section",
"title": "The July 14th, 2000 \"Bastille Day\" solar event as observed by Voyagers 1 and 2 in the distant heliosphere",
"author": [
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Heikkila",
"given_name": "B. C.",
"clpid": "Heikkila-B-C"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "Ness",
"given_name": "N. F.",
"clpid": "Ness-N-F"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Richardson",
"given_name": "J. D.",
"orcid": "0000-0003-4041-7540",
"clpid": "Richardson-J-D"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "One of the most powerful solar events observed over the current cycle occurred at 1024 July 14, 2000 accompanied by an X-5.7 x-ray burst and a full halo coronal mass ejection that initially was traveling at a velocity of > 1700 km/s. At earth the solar energetic particle event was the largest so far in cycle 23. Some 177 days later (2001.02) at V-2 (63 AU, 24\u00baS) there began a step decrease in the cosmic ray intensity (15% for 265 MeV/n GCR He) and a complex enhancement with multiple structure in the magnitude of the interplanetary magnetic field. For lowenergy 2.3 MeV protons there was a 10-fold increase in intensity that tracks the increase in the solar wind velocity which reached a peak value of ~450 km/s. This event is discussed in the context of the increases in intensity of MeV ions and the modulation events for galactic and anomalous cosmic rays that have been observed in the distant heliosphere for solar cycle 23 through 2001.4.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:hzest-tsn04",
"collection": "authors",
"collection_id": "hzest-tsn04",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150302-111956144",
"type": "book_section",
"title": "Inferring Energetic Particle Mean Free Paths from Observations of Anomalous Cosmic Rays in the Outer Heliosphere at Solar Maximum",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "We find that the mean free pathlength is higher by a factor of 10 or more at solar minimum than at the last solar maximum in 1900-1991, consistent with previous findings. In 2000-2001, the mean free pathlength has declined by a factor of ~10, but is still larger by a factor of ~3.6 than its value of ~0.15 AU in 1990-1991. As solar maximum conditions become durably established in the outer heliosphere over the next few months, it may be possible to deduce the radial dependence of the mean free pathlength.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:jjm0n-ep343",
"collection": "authors",
"collection_id": "jjm0n-ep343",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150226-150957759",
"type": "book_section",
"title": "Estimate of the Location of the Solar wind Termination Shock",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"abstract": "Over the next three years the termination shock is\nexpected to reach its minimum distance from the Sun before\nmoving outward again in response to increased solar wind\ndynamic pressure during the new solar cycle. Five different\nmethods of inferring the distance to the shock lead to estimates that cluster in the range of 90\u00b1 LO AU. In August 2001 Voyager I will be at 82 AU and moving outward at 3.6 AU\nper year, suggesting the possibility of encountering the termination shock by 2005 before it starts moving outward again.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "2001"
},
{
"id": "authors:4qa5f-kw436",
"collection": "authors",
"collection_id": "4qa5f-kw436",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-115932195",
"type": "article",
"title": "Cosmic-ray time scales using radioactive clocks",
"author": [
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Radionuclides in the galactic cosmic rays serve as chronometers for measuring the characteristic time of physical processes affecting cosmic ray energy spectra and composition. The radionuclide ^(59)Ni, present in the ejecta of supernovae, will decay to ^(59)Co via electron-capture with a halflife of T_(1/2) = 7.6 \u00d7 10^4 yr. However, if the cosmic ray acceleration time scale is shorter than the decay halflife, ^(59)Ni will become fully-stripped of electrons and will be present in the cosmic rays. Abundances of cosmic ray ^(59)Ni and ^(59)Co measured with the Cosmic Ray Isotope Spectrometer (CRIS) are consistent with the decay of all source ^(59)Ni, implying an acceleration time delay > 10^5 yr. Abundances of the \u03b2-decay radioactive secondaries, produced by fragmentation of the cosmic rays during transport in the interstellar medium (ISM), depend on the time scales for spallation and escape from the Galaxy. Consequently, measurement of these abundances can be used to derive the galactic confinement time, \u03c4_(esc), for cosmic rays. Using the abundances of the \u03b2-decay species ^(10)Be, ^(26)Al, ^(36)Cl, and ^(54)Mn measured by CRIS, we find a confinement time \u03c4_(esc) \u223c 15 Myr.",
"doi": "10.1016/S0273-1177(01)00114-4",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "2001",
"series_number": "4",
"volume": "27",
"issue": "4",
"pages": "727-736"
},
{
"id": "authors:pd9r4-j6345",
"collection": "authors",
"collection_id": "pd9r4-j6345",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-134629834",
"type": "book_section",
"title": "The Isotopic Composition of Cosmic-Ray Calcium",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "The isotopic composition of galactic cosmic-ray Ca has been measured over the energy range \u02dc 150 to 400 MeV/nuc on the Advanced Composition Explorer (ACE) mission. Using the measured abundances of the dominantly-secondary Ca isotopes with A = 41-46 as constraints, in combination with measured cross sections for the production of Ca isotopes by fragmentation of ^(56)Fe on hydrogen, we show that the two doubly-magic isotopes ^(40)Ca and ^(48)Ca consist mainly of primary material. We find that their relative abundances in the cosmic-ray source are very similar to those found in solar-system material, in spite of the fact that different types of stars are thought to be responsible for producing these two isotopes. This observation is consistent with the view that cosmic rays are derived from a mixed sample of interstellar matter.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:jv38d-6tn11",
"collection": "authors",
"collection_id": "jv38d-6tn11",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-131355783",
"type": "book_section",
"title": "Measurements of the Isotopes of Lithium, Beryllium, and Boron from ACE/CRIS",
"author": [
{
"family_name": "de Nolfo",
"given_name": "G. A.",
"orcid": "0000-0002-3677-074X",
"clpid": "de-Nolfo-G-A"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "The cosmic-ray isotopes of lithium, beryllium, and boron (LiBeB) are generally believed to originate from interactions within the interstellar medium, primarily through CNO spallation. Other sources are known to contribute to the abundance of ^7Li and ^(11)B, most notably the production of ^7Li from big bang nucleosynthesis. Thus, identifying the abundances of the galactic cosmic-ray LiBeB places important constraints on the interpretations of early epoch nucleosynthesis. The Cosmic Ray Isotope Spectrometer (CRIS) on ACE has been measuring isotopic composition from helium through zinc in the energy range \u02dc70-500 MeV/nucleon since 1997 with high statistical accuracy. We present measurements of the isotopic abundances of LiBeB from CRIS and discuss these observations in the context of previous cosmic-ray measurements and predictions from cosmic-ray transport models.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:y6dee-67g63",
"collection": "authors",
"collection_id": "y6dee-67g63",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150305-133531087",
"type": "book_section",
"title": "A Search for ^7Be in Solar Energetic Particle Events",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohls",
"given_name": "M.",
"clpid": "Pohls-M"
}
],
"abstract": "The LDEF spacecraft measured an unexpectedly high level of ^7Be, presumably swept up from the residual atmosphere. However, it is unclear whether the atmospheric ^7Be is due to particles originating in nuclear reachtions at the Sun, or due to secondary fragments from coll isions between energetic particles (solar and galactic) and the atmosphere. The Solar Isotope Spectrometer (SIS) on ACE has been measuring solar energetic particles since launch in 1997. We will present the results of a search for solar ^7Be\nabove about 5 MeV/nucleon with the SIS instrument.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:p2g6c-pjs66",
"collection": "authors",
"collection_id": "p2g6c-pjs66",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200506-160349946",
"type": "book_section",
"title": "The Origin of Primary Cosmic Rays: Constraints from ACE Elemental and Isotopic Composition Observations",
"book_title": "The Astrophysics of Galactic Cosmic Rays",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M-L"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Diehl",
"given_name": "Roland",
"clpid": "Diehl-R"
},
{
"family_name": "Parizot",
"given_name": "Etinenne",
"clpid": "Parizot-E"
},
{
"family_name": "Kallenbach",
"given_name": "Reinald",
"clpid": "Kallenbach-R"
},
{
"family_name": "von Steiger",
"given_name": "Rudolf",
"clpid": "von-Steiger-R"
}
],
"abstract": "Cosmic-ray isotope observations from NASA's Advanced Composition Explorer (ACE) mission have been used to investigate the composition of cosmic-ray source material. Source abundances relative to \u2075\u2076Fe are reported for eleven isotopes of Ca, Fe, Co, and Ni, including the very rare isotopes \u2074\u2078Ca and \u2076\u2074Ni. Although the source abundances range over a factor ~ 10\u2074, most of the ratios to \u2075\u2076Fe are consistent with solar-system values to within ~ 20%. However, there are some notable differences, the most significant being an excess of ~ (70 \u00b1 30)% relative to the solar system for the cosmic-ray source ratio \u2075\u2078Fe/\u2075\u2076Fe. The possible association of such an excess with a contribution to the cosmic-ray source from Wolf\u2014Rayet star ejecta is discussed.",
"doi": "10.1007/978-94-017-3239-0_2",
"isbn": "9789048158621",
"publisher": "Springer Netherlands",
"place_of_publication": "Dordrecht",
"publication_date": "2001",
"pages": "15-26"
},
{
"id": "authors:kb0sy-xwx26",
"collection": "authors",
"collection_id": "kb0sy-xwx26",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150302-112545330",
"type": "book_section",
"title": "High Energy Ionic Charge State Composition in Large Solar Energetic Particle Events",
"author": [
{
"family_name": "Labrador",
"given_name": "A. W.",
"orcid": "0000-0001-9178-5349",
"clpid": "Labrador-A-W"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-M"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "Measurements of ionic charge states in solar energetic particle (SEP) events have been made at relatively high energies (> 15 MeV/nucleon) with the Mass Spectrometer Telescope (MAST) on board the Solar, Anomalous, and Magnetospheric Particle Explorer (SAMPEX) satellite using the Earth's magnetic field as a particle rigidity filter. We have examined the largest SEP events of solar cycle 23 and determined ionic charge states of Fe and other elements in several of these events. The mean charge state of Fe is often considerably higher (~20) in impulsive SEP events than in gradual events (~15). Surprisingly, in several cases, relatively high charge states of around 20 were found for Fe in very large events which are most likely gradual. Further, our measurements also show that Si in these events is not necessarily in thermal equilibrium with other elements.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:ad6pb-g2f38",
"collection": "authors",
"collection_id": "ad6pb-g2f38",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-133259423",
"type": "book_section",
"title": "The Cosmic-Ray Contribution to LiBeB: Interpretation of LiBeB Abundances from CRIS",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-Manfred"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "The bulk of galactic Li, Be, and B (LiBeB) abundances is believed to be created during energetic inelastic collisions of cosmic-ray and interstellar medium (ISM) nuclei. Additional sources such as big bang nucleosynthesis or neutrino-driven spallation within Type II supernovae may also add a small contribution. However, measurements of the elemental ratios Be/H, B/H, and Fe/H in old, low-metallicity halo stars indicate an overabundance of LiBeB that can not be accounted for by fragmentation of cosmic-ray CNO. This interpretation assumes that the ISM in any epoch serves as a source of material both for star formation and for cosmic rays, which contribute fragmentation material in later epochs. We have simulated cosmic-ray transport using a simple model and present an interpretation of the abundance measurements from the Cosmic Ray Isotope Spectrometer (CRIS) during the past three years. We will discuss the implications on cosmic-ray LiBeB production at lower energies.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:tb6er-82z45",
"collection": "authors",
"collection_id": "tb6er-82z45",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-135509933",
"type": "book_section",
"title": "CRIS Measurements of Electron-Capture-Decay Isotopes: ^(37)Ar, ^(44)Ti, ^(49)V, ^(51)Cr, ^(55)Fe, and ^(57)Co",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Simon",
"given_name": "M.",
"clpid": "Simon-Manfred"
},
{
"family_name": "Lorenz",
"given_name": "E.",
"clpid": "Lorenz-E"
},
{
"family_name": "Pohl",
"given_name": "M.",
"clpid": "Pohl-M"
}
],
"abstract": "The secondary isotopes ^(37)Ar, ^(44)Ti, ^(49)V, ^(51)Cr, ^(55)Fe, and ^(57)Co decay only by electron capture, which occurs preferentially at the lower cosmic-ray energies, where electron attachment is more likely. Measurements of the abundances of these isotopes may reveal the interstellar energies of cosmic rays during propagation and whether reacceleration occurred. Stable secondary isotopes may also be used to examine energy dependence and reacceleration. The Cosmic Ray Isotope Spectrometer has detected large numbers of these nuclei at 100 - 500 MeV/nucleon during a time spanning solar minimum and solar maximum, allowing an additional study of solar modulation. This paper will discuss several subiron abundance ratios and the implications for reacceleration and solar modulation.",
"publisher": "Copernicus Systems and Technology GmbH",
"publication_date": "2001"
},
{
"id": "authors:432n3-p3436",
"collection": "authors",
"collection_id": "432n3-p3436",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111201-093810051",
"type": "book_section",
"title": "Constraints on cosmic-ray acceleration and transport from isotope observations",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Miller",
"given_name": "Marjorie",
"clpid": "Miller-M"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "Martin A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Zurbuchen",
"given_name": "Thomas H.",
"clpid": "Zurbuchen-T-H"
},
{
"family_name": "Mobius",
"given_name": "Eberhard",
"clpid": "Mobius-E"
}
],
"abstract": "Observations from the Cosmic Ray Isotope Spectrometer (CRIS) on ACE have been used to derive constraints on the locations, physical conditions, and time scales for cosmic-ray acceleration and transport. The isotopic composition of Fe, Co, and Ni is very similar to that of solar system material, indicating that cosmic rays contain contributions from supernovae of both Type II and Type Ia. The electron-capture primary ^(59)Ni produced in supernovae has decayed, demonstrating that a time \u227310^5 yr elapses before acceleration of the bulk of the cosmic rays and showing that most of the accelerated material is derived from old stellar or interstellar material rather than from fresh supernova ejecta.",
"doi": "10.1063/1.1324340",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, New York",
"publication_date": "2000-09-15",
"pages": "363-370"
},
{
"id": "authors:p6ht5-y7g83",
"collection": "authors",
"collection_id": "p6ht5-y7g83",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111215-092255591",
"type": "book_section",
"title": "The Solar Energetic Particle Event of 6 May 1998",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "M. A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Mobius",
"given_name": "E.",
"clpid": "Mobius-E"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
}
],
"abstract": "The abundances of elements from helium to iron have been measured in more than a dozen moderate to large solar energetic particle (SEP) events using the Solar Isotope Spectrometer (SIS) on-board the Advanced Composition Explorer (ACE). Time variations within some of these events and from event to event have been reported previously. This paper presents an analysis of the event of 6 May 1998, for which relatively time-independent abundance ratios are found. This event has been considered to be an example of an impulsive event, a gradual event, and as a hybrid of the two. Difficulties with classifying this event are discussed.",
"doi": "10.1063/1.1324291",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "111-114"
},
{
"id": "authors:hqg5f-a5008",
"collection": "authors",
"collection_id": "hqg5f-a5008",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111123-095344770",
"type": "book_section",
"title": "Galactic Cosmic Ray Neon Isotopic Abundances Measured on ACE",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Niebur",
"given_name": "S. M.",
"clpid": "Niebur-S-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "M. A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Mobius",
"given_name": "E.",
"clpid": "Mobius-E"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
}
],
"abstract": "Measurements of neon isotopic abundances from the ACE-CRIS experiment are presented. Abundances have been obtained in six energy intervals over the energy range of ~100\u2264E\u2264280 MeV/nucleon. These measurements are compared with the ACE-SIS data for lower energies extending down to ~8 MeV/nucleon. We find that the CRIS ^(22)Ne/^(20)Ne abundance ratio at the source is a factor of 5.0\u00b10.3 greater than for the solar wind. The CRIS measured abundances agree well with previous experiments. The CRIS and SIS measurements are in good agreement for the higher SIS energies. However for the lower energy SIS data, where the anomalous cosmic rays (ACR) are being sampled, the ratio decreases and agrees with solar wind abundances. The implications of these results are discussed.",
"doi": "10.1063/1.1324349",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "413-416"
},
{
"id": "authors:h5tg9-wvt05",
"collection": "authors",
"collection_id": "h5tg9-wvt05",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111209-071511880",
"type": "book_section",
"title": "Variable fractionation of solar energetic particles according to first ionization potential",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Miller",
"given_name": "M.",
"clpid": "Miller-M"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "Martin A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Zurbuchen",
"given_name": "Thomas H.",
"clpid": "Zurbuchen-T-H"
},
{
"family_name": "Mobius",
"given_name": "Eberhard",
"clpid": "Mobius-E"
}
],
"abstract": "The average composition of solar energetic particles (SEPs), like the solar corona, is known to be depleted in elements with first ionization potential (FIP) more than ~10 eV by a factor of approximately four. We examine evidence for event to event variations in the FIP-related fractionation of SEPs, following up a 1994 study by Garrard and Stone. In a survey of 46 SEP events from 1974 to 1999 the deduced FIP-fractionation varies by a factor of ~2 from event to event, with no apparent relation to charge-to-mass dependent fractionation patterns in these same events. These results are compared to similar variations observed in the solar wind.",
"doi": "10.1063/1.1324294",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "123-126"
},
{
"id": "authors:zghem-kq516",
"collection": "authors",
"collection_id": "zghem-kq516",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150219-131410930",
"type": "book_section",
"title": "Secondary Electron-Capture-Decay Isotopes and Implications for the Propagation of Galactic Cosmic rays",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Niebur",
"given_name": "S. M.",
"clpid": "Niebur-S-M"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Israel",
"given_name": "M. H.",
"orcid": "0000-0002-8104-208X",
"clpid": "Israel-M-H"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Miller",
"given_name": "Marjorie",
"clpid": "Miller-M"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "Martin A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
},
{
"family_name": "M\u00f6bius",
"given_name": "E.",
"clpid": "M\u00f6bius-E"
}
],
"abstract": "We report the first observation of an energy dependence in the titanium, vanadium, and chromium isotopic abundances in cosmic rays. The observations were made in the 100\u2013500 MeV/nucleon energy interval using data from the Cosmic Ray Isotope Spectrometer on the ACE spacecraft. The ^(51)Cr and ^(49)V isotopes in cosmic rays are produced by fragmentation of heavier cosmic ray nuclides and decay only by electron capture. The observations indicate that electron-capture decay occurred primarily at the lower energies measured, and that there is a resulting energy dependence in the abundances of these isotopes and their decay products.",
"doi": "10.1063/1.1324347",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "406-409"
},
{
"id": "authors:eb0jn-bxr08",
"collection": "authors",
"collection_id": "eb0jn-bxr08",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150219-135833866",
"type": "book_section",
"title": "On the Low Energy Decrease in Galactic Cosmic Ray Secondary/Primary Ratios",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Miller",
"given_name": "Marjorie",
"clpid": "Miller-M"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "Martin A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
},
{
"family_name": "M\u00f6bius",
"given_name": "E.",
"clpid": "M\u00f6bius-E"
}
],
"abstract": "Galactic cosmic ray (GCR) secondary/primary ratios such as B/C and (Sc+Ti+V)/Fe are commonly used to determine the mean amount of interstellar material through which cosmic rays travel before escaping from the Galaxy (\u039besc). These ratios are observed to be energy-dependent, with a relative maximum at \u223c1 GeV/nucleon, implying a corresponding peak in \u039besc. The decrease in \u039b_(esc) at energies above 1 GeV/nucleon is commonly taken to indicate that higher energy cosmic rays escape more easily from the Galaxy. The decrease in \u039b_(esc) at energies <1 GeV/nuc is more controversial; suggested possibilities include the effects of a galactic wind or the effects of distributed acceleration of cosmic rays as they pass through the interstellar medium. We consider two possible explanations for the low energy decrease in \u039b_(esc) and attempt to fit the combined, high-resolution measurements of secondary/primary ratios from \u223c0.1 to 35 GeV/nuc made with the CRIS instrument on ACE and the C2 experiment on HEAO-3. The first possibility, which hypothesizes an additional, local component of low-energy cosmic rays that has passed through very little material, is found to have difficulty simultaneously accounting for the abundance of both B and the Fe-secondaries. The second possibility, suggested by Soutoul and Ptuskin, involves a new form for \u039b_(esc) motivated by their diffusion-convection model of cosmic rays in the Galaxy. Their suggested form for \u039b_(esc)(E) is found to provide an excellent fit to the combined ACE and HEAO data sets.",
"doi": "10.1063/1.1324351",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "421-428"
},
{
"id": "authors:mhqg7-78214",
"collection": "authors",
"collection_id": "mhqg7-78214",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150219-134914101",
"type": "book_section",
"title": "Abundances of the cosmic ray \u03b2-decay secondaries and implications for cosmic ray transport",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Yanasak",
"given_name": "N.",
"clpid": "Yanasak-N"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Jocipii",
"given_name": "J. R.",
"clpid": "Jocipii-J-R"
},
{
"family_name": "Lee",
"given_name": "M. A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Moebius",
"given_name": "E.",
"clpid": "Moebius-E"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
}
],
"abstract": "Galactic cosmic rays (GCRs) pass through the interstellar medium (ISM) and undergo nuclear interactions that produce secondary fragments. The abundances of radioactive secondary species can be used to derive a galactic\nconfinement time for cosmic rays using the amount of ISM material traversed by the cosmic rays inferred from stable\nGCR secondary abundances. Abundance measurements of long-lived species such as ^(10)Be, ^(26)Al, ^(36)Cl, and ^(54)Mn allow\na comparison of propagation histories for different parent nuclei. Abundances for these species, measured in the energy\nrange ~ 50 - 500 MeV/nuc using the Cosmic Ray Isotope Spectrometer (CRIS) aboard the Advanced Composition\nExplorer (ACE) spacecraft, indicate a confinement time \u03c4(esc) 16.2\u00b10.8 Myr. We have modeled the production and\npropagation of the radioactive secondaries and discuss the implications for GCR transport.",
"doi": "10.1063/1.1324346",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2000-09-15",
"pages": "402-405"
},
{
"id": "authors:3pb2g-6ng48",
"collection": "authors",
"collection_id": "3pb2g-6ng48",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111216-080137898",
"type": "book_section",
"title": "Enhanced Abundances of ^3He in Large Solar Energetic Particle Events",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "Martin A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Mobius",
"given_name": "Eberhard",
"clpid": "Mobius-E"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
}
],
"abstract": "Observations of a number of relatively large solar energetic particle (SEP) events that have occurred since the launch of ACE in August 1997 have shown that the ratio of ^3He/^4He can be enhanced over the solar wind value (~4\u00d710^(\u20134)) by more than an order of magnitude in such events. Since particle acceleration in these \"gradual\" SEP events is thought to be caused by CME-driven shocks traveling through the solar corona and interplanetary medium, a source of ^3He in addition to the solar wind appears required to provide the seed material. Using data from the Solar Isotope Spectrometer on ACE, we have carried out a more detailed investigation of the characteristics of the ^3He enhancements at energies >5 MeV/nucleon in three large SEP events (4 Nov 1997, 6 May 1998, and 14 Nov 1998). We find that the ^3He/^4He ratios are essentially time-independent during the events, that the ^3He energy spectra are markedly harder than those commonly observed in impulsive events, and that the spectra of ^3He may be harder than those of ^4He.",
"doi": "10.1063/1.1324290",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "107-110"
},
{
"id": "authors:kd7n0-gw612",
"collection": "authors",
"collection_id": "kd7n0-gw612",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111215-101637088",
"type": "book_section",
"title": "Measurements of Heavy Elements in ^3He-rich SEP Events",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"clpid": "Mewaldt-R-A"
}
],
"abstract": "Using the Solar Isotope Spectrometer (SIS) on the Advanced Composition Explorer (ACE), we have studied the properties of a selection of small ^3He-rich solar energetic particle (SEP) events with heavy ion enhancements in the energy range ~11\u201322 MeV/nucleon. These events contain significantly increased ^3He/^4He ratios over the solar wind value of 0.0004 in the energy range ~4.5\u20135.5 MeV/nucleon. In order to characterize the events, the following features have been investigated. First, the heavy element content has been measured and compared to that found in past studies of impulsive SEP events. Next, the simultaneous 38\u201353 keV electron flux, measured with the Electron, Proton, and Alpha Monitor (EPAM) on ACE, has been examined for possible activity near the ^3He-rich event onset times. Finally a list of measured solar X-ray flares, with corresponding H-alpha flares where possible, has been scrutinized for potential correlations with these events. The results show an apparent correlation between event onset and increased electron flux, and a possible association with X-ray flares.",
"doi": "10.1063/1.1324289",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "103-106"
},
{
"id": "authors:nzqcw-g9z69",
"collection": "authors",
"collection_id": "nzqcw-g9z69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111123-142326519",
"type": "book_section",
"title": "On the Low Energy Decrease in Galactic Cosmic Ray\n Secondary/Primary Ratios",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Davis",
"given_name": "A. J.",
"clpid": "Davis-A-J"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "M. A.",
"clpid": "Lee-M-A"
},
{
"family_name": "M\u00f6bius",
"given_name": "E.",
"clpid": "M\u00f6bius-E"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
}
],
"abstract": "Galactic cosmic ray (GCR) secondary/primary ratios such as B/C and (Sc+Ti+V)/Fe are commonly used to determine the mean amount of interstellar material through which cosmic rays travel before escaping from the Galaxy (\u039b_(esc)). These ratios are observed to be energy-dependent, with a relative maximum at ~1 GeV/nucleon, implying a corresponding peak in \u039b_(esc). The decrease in \u039b_(esc) at energies above 1 GeV/nucleon is commonly taken to indicate that higher energy cosmic rays escape more easily from the Galaxy. The decrease in \u039b_(esc) at energies <1 GeV/nuc is more controversial; suggested possibilities include the effects of a galactic wind or the effects of distributed acceleration of cosmic rays as they pass through the interstellar medium. We consider two possible explanations for the low energy decrease in \u039b_(esc) and attempt to fit the combined, high-resolution measurements of secondary/primary ratios from ~0.1 to 35 GeV/nuc made with the CRIS instrument on ACE and the C2 experiment on HEAO-3. The first possibility, which hypothesizes an additional, local component of low-energy cosmic rays that has passed through very little material, is found to have difficulty simultaneously accounting for the abundance of both B and the Fe-secondaries. The second possibility, suggested by Soutoul and Ptuskin, involves a new form for \u039b_(esc) motivated by their diffusion-convection model of cosmic rays in the Galaxy. Their suggested form for \u039b_(esc)(E) is found to provide an excellent fit to the combined ACE and HEAO data sets.",
"doi": "10.1063/1.1324351",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "421-424"
},
{
"id": "authors:tnmxh-ehz56",
"collection": "authors",
"collection_id": "tnmxh-ehz56",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111208-100352581",
"type": "book_section",
"title": "Observations of Anomalous Cosmic Rays at 1 AU",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "M. A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Mobius",
"given_name": "E.",
"clpid": "Mobius-E"
},
{
"family_name": "Zurbuchen",
"given_name": "T. H.",
"clpid": "Zurbuchen-T-H"
}
],
"abstract": "Anomalous cosmic rays (ACRs) provide a sensitive probe of the access of energetic particles to the inner heliosphere, varying in intensity by more than two orders of magnitude during the course of the solar cycle. New data which are becoming available from the Advanced Composition Explorer (ACE) can provide a detailed record of ACR intensity and spectral changes on short (~ 1 day) time scales during the approach to solar maximum, which will help address issues of ACR modulation and transport. The elemental and isotopic composition of ACRs provides important information on the source or sources of these particles, while their ionic charge state composition and its energy dependence\nserves as a diagnostic of their acceleration time scale. We review measurements of the ACR elemental, isotopic,\nand charge state composition and spectra as determined at 1 AU by SAMPEX, ACE, Wind, and other spacecraft. These\nresults are important input to models of the acceleration, modulation, and transport of ACRs.",
"doi": "10.1063/1.1324328",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "293-300"
},
{
"id": "authors:qh8qt-etk47",
"collection": "authors",
"collection_id": "qh8qt-etk47",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111123-124917397",
"type": "book_section",
"title": "The Isotopic Composition of Solar Energetic Particles",
"book_title": "Acceleration and Transport of Energetic Particles Observed in the Heliosphere",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"clpid": "Mewaldt-R-A"
}
],
"abstract": "Since the launch of ACE in August 1997, the Solar Isotope Spectrometer (SIS) has observed 11 large solar particle events in which elemental and isotopic composition was determined over a large energy range. The composition of these events has raised many issues and challenged generally accepted characterizations of solar energetic particle (SEP) events. In particular, ^3He/^4He enhancements have been observed in several large events as well as enhancements of heavy ions typically associated with smaller impulsive events. The isotopic composition varies substantially from event to event (a factor of 3 for ^(22)Ne/^(20)Ne) with enhancements and depletions that are generally correlated with elemental composition. This correlation suggests that the isotopic enhancements may be related to the Q/M fractionation typically evident in the elemental composition of SEP events. However, there are also significant deviations from this pattern, which may imply that wave-particle resonances or other mass fractionation processes may be involved. We review the recent isotopic observations made with ACE and discuss their implications for particle acceleration and transport.",
"doi": "10.1063/1.1324281",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, N.Y.",
"publication_date": "2000-09-15",
"pages": "55-62"
},
{
"id": "authors:6vs9s-dcp02",
"collection": "authors",
"collection_id": "6vs9s-dcp02",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140225-104036311",
"type": "article",
"title": "Solar cycle dependence of the geomagnetically trapped anomalous cosmic rays",
"author": [
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
}
],
"abstract": "Solar cycle variations in the intensity of geomagnetically trapped anomalous cosmic ray (ACR) oxygen are demonstrated by \u223c7 years of data from the SAMPEX satellite. They correspond to similar variations in the interplanetary ACR source. Trapped particle losses during the approach to solar maximum are not associated with geomagnetic activity and may be consistent with atmospheric energy degradation. The average trapped particle pitch angle distribution and energy spectra support this interpretation in which both source and loss rates are proportional to atmospheric density.",
"doi": "10.1029/2000GL000049",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "2000-08-01",
"series_number": "15",
"volume": "27",
"issue": "15",
"pages": "2349-2352"
},
{
"id": "authors:0eewn-xz288",
"collection": "authors",
"collection_id": "0eewn-xz288",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:ABUprl00",
"type": "article",
"title": "Exclusion limits on the WIMP-nucleon cross section from the Cryogenic Dark Matter Search",
"author": [
{
"family_name": "Abusaidi",
"given_name": "R.",
"clpid": "Abusaidi-R"
},
{
"family_name": "Akerib",
"given_name": "D. S.",
"clpid": "Akerib-D-S"
},
{
"family_name": "Barnes",
"given_name": "P. D., Jr.",
"clpid": "Barnes-P-D-Jr"
},
{
"family_name": "Bauer",
"given_name": "D. A.",
"clpid": "Bauer-D-A"
},
{
"family_name": "Bolozdynya",
"given_name": "A.",
"clpid": "Bolozdynya-A"
},
{
"family_name": "Brink",
"given_name": "P. L.",
"clpid": "Brink-P-L"
},
{
"family_name": "Bunker",
"given_name": "R.",
"clpid": "Bunker-R"
},
{
"family_name": "Cabrera",
"given_name": "B.",
"clpid": "Cabrera-B"
},
{
"family_name": "Caldwell",
"given_name": "D. O.",
"clpid": "Caldwell-D-O"
},
{
"family_name": "Castle",
"given_name": "J. P.",
"clpid": "Castle-J-P"
},
{
"family_name": "Clarke",
"given_name": "R. M.",
"clpid": "Clarke-R-M"
},
{
"family_name": "Colling",
"given_name": "P.",
"clpid": "Colling-P"
},
{
"family_name": "Crisler",
"given_name": "M. B.",
"clpid": "Crisler-M-B"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Da Silva",
"given_name": "A.",
"clpid": "Da-Silva-A"
},
{
"family_name": "Davies",
"given_name": "A. K.",
"clpid": "Davies-A-K"
},
{
"family_name": "Dixon",
"given_name": "R.",
"clpid": "Dixon-R"
},
{
"family_name": "Dougherty",
"given_name": "B. L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Driscoll",
"given_name": "D.",
"clpid": "Driscoll-D"
},
{
"family_name": "Eichblatt",
"given_name": "S.",
"clpid": "Eichblatt-S"
},
{
"family_name": "Emes",
"given_name": "J.",
"clpid": "Emes-J"
},
{
"family_name": "Gaitskell",
"given_name": "R. J.",
"clpid": "Gaitskell-R-J"
},
{
"family_name": "Golwala",
"given_name": "S. R.",
"orcid": "0000-0002-1098-7174",
"clpid": "Golwala-S-R"
},
{
"family_name": "Hale",
"given_name": "D.",
"clpid": "Hale-D"
},
{
"family_name": "Haller",
"given_name": "E. E.",
"clpid": "Haller-E-E"
},
{
"family_name": "Hellmig",
"given_name": "J.",
"clpid": "Hellmig-J"
},
{
"family_name": "Huber",
"given_name": "M. E.",
"clpid": "Huber-M-E"
},
{
"family_name": "Irwin",
"given_name": "K. D.",
"clpid": "Irwin-K-D"
},
{
"family_name": "Jochum",
"given_name": "J.",
"clpid": "Jochum-J"
},
{
"family_name": "Lipschultz",
"given_name": "F. P.",
"clpid": "Lipschultz-F-P"
},
{
"family_name": "Lu",
"given_name": "A.",
"clpid": "Lu-A"
},
{
"family_name": "Mandic",
"given_name": "V.",
"clpid": "Mandic-V"
},
{
"family_name": "Martinis",
"given_name": "J. M.",
"clpid": "Martinis-J-M"
},
{
"family_name": "Nam",
"given_name": "S. W.",
"clpid": "Nam-S-W"
},
{
"family_name": "Nelson",
"given_name": "H.",
"clpid": "Nelson-H"
},
{
"family_name": "Neuhauser",
"given_name": "B.",
"clpid": "Neuhauser-B"
},
{
"family_name": "Penn",
"given_name": "M. J.",
"clpid": "Penn-M-J"
},
{
"family_name": "Perera",
"given_name": "T. A.",
"clpid": "Perera-T-A"
},
{
"family_name": "Isaac",
"given_name": "M. C. Perillo",
"clpid": "Isaac-M-C-P"
},
{
"family_name": "Pritychenko",
"given_name": "B.",
"clpid": "Pritychenko-B"
},
{
"family_name": "Ross",
"given_name": "R. R.",
"clpid": "Ross-R-R"
},
{
"family_name": "Saab",
"given_name": "T.",
"clpid": "Saab-T"
},
{
"family_name": "Sadoulet",
"given_name": "B.",
"clpid": "Sadoulet-B"
},
{
"family_name": "Schnee",
"given_name": "R. W.",
"clpid": "Schnee-R-W"
},
{
"family_name": "Seitz",
"given_name": "D. N.",
"clpid": "Seitz-D-N"
},
{
"family_name": "Shestople",
"given_name": "P.",
"clpid": "Shestople-P"
},
{
"family_name": "Shutt",
"given_name": "T.",
"clpid": "Shutt-T"
},
{
"family_name": "Smith",
"given_name": "A.",
"orcid": "0000-0002-1938-4660",
"clpid": "Smith-A"
},
{
"family_name": "Smith",
"given_name": "G. W.",
"clpid": "Smith-G-W"
},
{
"family_name": "Sonnenschein",
"given_name": "A. H.",
"clpid": "Sonnenschein-A-H"
},
{
"family_name": "Spadafora",
"given_name": "A. L.",
"clpid": "Spadafora-A-L"
},
{
"family_name": "Stockwell",
"given_name": "W.",
"clpid": "Stockwell-W"
},
{
"family_name": "Taylor",
"given_name": "J. D.",
"clpid": "Taylor-J-D"
},
{
"family_name": "White",
"given_name": "S.",
"clpid": "White-S"
},
{
"family_name": "Yellin",
"given_name": "S.",
"clpid": "Yellin-S"
},
{
"family_name": "Young",
"given_name": "B. A.",
"clpid": "Young-B-A"
},
{
"literal": "CDMS Collaboration"
}
],
"abstract": "The Cryogenic Dark Matter Search (CDMS) employs Ge and Si detectors to search for weakly interacting massive particles (WIMPs) via their elastic-scattering interactions with nuclei while discriminating against interactions of background particles. CDMS data, accounting for the neutron background, give limits on the spin-independent WIMP-nucleon elastic-scattering cross section that exclude unexplored parameter space above 10 GeV/c^2 WIMP mass and, at >75% C.L., the entire 3\u03c3 allowed region for the WIMP signal reported by the DAMA experiment.",
"doi": "10.1103/PhysRevLett.84.5699",
"issn": "0031-9007",
"publisher": "American Physical Society",
"publication": "Physical Review Letters",
"publication_date": "2000-06-19",
"series_number": "25",
"volume": "84",
"issue": "25",
"pages": "5699-5703"
},
{
"id": "authors:qgppk-yjp74",
"collection": "authors",
"collection_id": "qgppk-yjp74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-100748785",
"type": "book_section",
"title": "Cosmic Ray Source Abundances and the Acceleration of Cosmic Rays",
"book_title": "ACE 2000 Symposium",
"author": [
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Barghouty",
"given_name": "A. F.",
"clpid": "Barghouty-A-F"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Miller",
"given_name": "Marjorie",
"clpid": "Miller-M"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Lee",
"given_name": "Martin A.",
"clpid": "Lee-M-A"
},
{
"family_name": "Zurbuchen",
"given_name": "Thomas H.",
"clpid": "Zurbuchen-T-H"
},
{
"family_name": "Mobius",
"given_name": "Eberhard",
"clpid": "Mobius-E"
}
],
"abstract": "The galactic cosmic ray elemental source abundances display a fractionation that is possibly based on first ionization potential (FIP) or volatility. A few elements break the general correlation of FIP and volatility and the abundances of these may help to distinguish between models for the origin of the cosmic ray source material. Data from the Cosmic Ray Isotope Spectrometer instrument on NASA's Advanced Composition Explorer spacecraft were used to derive source abundances for several of these elements (Na, Cu, Zn, Ga, Ge). Three (Na, Cu, Ge) show depletions which could be consistent with a volatility-based source fractionation model.",
"doi": "10.1063/1.1324355",
"isbn": "1-56396-951-3",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "2000-01",
"pages": "437-440"
},
{
"id": "authors:kt7gz-8wn91",
"collection": "authors",
"collection_id": "kt7gz-8wn91",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-071624732",
"type": "book_section",
"title": "Measurements of the Heavy-Ion Elemental and Isotopic Composition in Large Solar Particle Events from ACE",
"book_title": "High Energy Solar Physics - Anticipating HESSI",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Ramaty",
"given_name": "R.",
"clpid": "Ramaty-R"
},
{
"family_name": "Mandzhavidze",
"given_name": "N.",
"clpid": "Mandzhavidze-N"
}
],
"abstract": "Using the Solar Isotope Spectrometer (SIS) on the Advanced\nComposition Explorer (ACE), we have measured the isotopic composition of as many as eleven elements from He through Ni at energies of tens of MeV /nucleon in eleven solar energetic particle (SEP) events that have occurred since November 1997. We find that isotopic composition varies dramatically from event to event. For example, the ^(22)Ne/^(20)Ne ratio ranges from ~ 0. 7 to > 2 times the solar wind value, being lowest for iron-poor events and highest for iron-rich events. We present the SIS SEP isotope measurements to date and show that the strong correlation of elemental and isotopic abundance ratios suggests that elemental and isotopic fractionation are governed by the same process.",
"isbn": "1-58381-033-1",
"publisher": "Astronomical Society of the Pacific",
"place_of_publication": "San Francisco, CA",
"publication_date": "2000",
"pages": "118-123"
},
{
"id": "authors:sv6jn-t8227",
"collection": "authors",
"collection_id": "sv6jn-t8227",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140826-080801901",
"type": "book_section",
"title": "Observations of ^3He-rich Solar Energetic Particle Events with the Solar Isotope Spectrometer",
"book_title": "High Energy Solar Physics - Anticipating HESSI",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Ramaty",
"given_name": "R.",
"clpid": "Ramaty-R"
},
{
"family_name": "Mandzhavidze",
"given_name": "N.",
"clpid": "Mandzhavidze-N"
}
],
"abstract": "Using ~4 MeV /nucleon solar energetic particle data from\nthe Solar Isotope Spectrometer (SIS) on the Advanced Composition Explorer (ACE), we identify 60 ^3He-rich time periods longer than 5 hours in length. As many of these time periods do not have \"classical\" impulsive profiles, we classify each event as one of 4 event types (based on the morphology of the event). The time periods have been associated with solar events listed by the Space Environment Center and energetic electron events observed by the Electron, Proton, and Alpha Monitor (EPAM) on\nACE. Only half of the events could be associated with an x-ray event and 63% with an electron event.",
"isbn": "1-58381-033-1",
"publisher": "Astronomical Society of the Pacific",
"place_of_publication": "San Francisco, CA",
"publication_date": "2000",
"pages": "124-129"
},
{
"id": "authors:z2k7x-f9s78",
"collection": "authors",
"collection_id": "z2k7x-f9s78",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140902-132158815",
"type": "article",
"title": "Constraints on the Time Delay between Nucleosynthesis and Cosmic-Ray Acceleration from Observations of ^(59)Ni and ^(59)Co",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dougherty",
"given_name": "B. L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Thayer",
"given_name": "M. R.",
"clpid": "Thayer-M-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"abstract": "Measurements of the abundances of cosmic-ray ^(59)Ni and ^(59)Co are reported from the Cosmic-Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer. These nuclides form a parent-daughter pair in a radioactive decay which can occur only by electron capture. This decay cannot occur once the nuclei are accelerated to high energies and stripped of their electrons. The CRIS data indicate that the decay of ^(59)Ni to ^(59)Co has occurred, leading to the conclusion that a time longer than the 7.6 \u00d7 10^4 yr half-life of ^(59)Ni elapsed before the particles were accelerated. Such long delays indicate the acceleration of old, stellar or interstellar material rather than fresh supernova ejecta. For cosmic-ray source material to have the composition of supernova ejecta would require that these ejecta not undergo significant mixing with normal interstellar gas before ~10^5 yr has elapsed.",
"doi": "10.1086/312242",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "1999-09-20",
"series_number": "1",
"volume": "523",
"issue": "1",
"pages": "L61-L64"
},
{
"id": "authors:77c1s-a3b69",
"collection": "authors",
"collection_id": "77c1s-a3b69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140828-090809602",
"type": "article",
"title": "Event-to-event variations in the isotopic composition of neon in solar energetic particle events",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Using the Solar Isotope Spectrometer on the Advanced Composition Explorer, we have measured the isotopic composition of neon at 24\u201372 MeV/nucleon in nine solar energetic particle events between 4 November 1997 and 16 November 1998. The ^(22)Ne/^(20)Ne ratio varies from \u223c0.7 to \u223c2 times the solar wind value from event to event, indicating significant mass fractionation in the acceleration and/or transport of these particles. The mass fractionation is strongly correlated with the Fe/O and Na/Mg element abundance ratios, suggesting that elemental and isotopic fractionation are both governed by the ionic charge to mass ratio.",
"doi": "10.1029/1999GL900561",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1999-09-01",
"series_number": "17",
"volume": "26",
"issue": "17",
"pages": "2693-2696"
},
{
"id": "authors:taehd-0mp12",
"collection": "authors",
"collection_id": "taehd-0mp12",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-151845333",
"type": "article",
"title": "New observations of heavy-ion-rich solar particle events from ACE",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Following launch of the Advanced Composition Explorer in August 1997, the Solar Isotope Spectrometer measured the composition of nine solar energetic particle events. We have used isotopic measurements of Ne to determine the degree of charge-to-mass-dependent fractionation and infer the charge states of C-Ni in the four most heavy-ion-rich of the nine events. The results indicate a source temperature of \u223c4\u00d710^6 K; this and the measured abundances suggest that these four events are more characteristic of impulsive events than gradual. Although the ^3He/^4He ratios are not enhanced to the level commonly ascribed to impulsive events, there are sizable enhancements over typical solar wind values measured in three of the events.",
"doi": "10.1029/1999GL900560",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1999-09-01",
"series_number": "17",
"volume": "26",
"issue": "17",
"pages": "2697-2700"
},
{
"id": "authors:ta3xp-ts246",
"collection": "authors",
"collection_id": "ta3xp-ts246",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140819-132327153",
"type": "book_section",
"title": "Estimating Characteristics of the Heliosphere Using Anomalous Cosmic Ray Observations at Solar Maximum",
"book_title": "The solar wind nine conference",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"contributor": [
{
"family_name": "Habbal",
"given_name": "S. R.",
"clpid": "Habbal-S-R"
},
{
"family_name": "Esser",
"given_name": "R.",
"clpid": "Esser-R"
},
{
"family_name": "Hollweg",
"given_name": "J. V.",
"clpid": "Holweg-J-V"
},
{
"family_name": "Isenberg",
"given_name": "P. A.",
"clpid": "Isenberg-P-A"
}
],
"abstract": "Observations of the energy spectra of anomalous cosmic ray (ACR) oxygen were acquired in the outer heliosphere during the last solar maximum period in 1990 when the particle distributions are expected to be more nearly spherically symmetric than at solar minimum. Hence, we use a simple one-dimensional model of ACR acceleration and transport to fit the observed energy spectra at Voyagers 1 and 2 and Pioneer 10. The inferred interplanetary radial diffusion coefficient is remarkably consistent with recent theoretical estimates. The next solar maximum is expected to occur in the outer heliosphere in early 2001 when Voyager 1 will be \u223c80 AU from the Sun. We predict that the intensity of ACR oxygen and helium at Voyagers 1 and 2 will be sufficiently large, and the model uncertainties sufficiently small, that it should be possible in 2001 to determine the remaining distance to the shock to within \u00b11 AU if the shock is within \u223c5 AU, \u22123 to +6 AU if the shock is within \u223c15 AU, and \u22125 to +14 AU if the shock is within \u223c25 AU.",
"doi": "10.1063/1.58794",
"isbn": "1563968657",
"publisher": "American Institute of Physics",
"place_of_publication": "Melville, NY",
"publication_date": "1999-06-16",
"pages": "201-204"
},
{
"id": "authors:k0xp3-78g73",
"collection": "authors",
"collection_id": "k0xp3-78g73",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-130259341",
"type": "article",
"title": "Particle acceleration and sources in the November 1997 solar energetic particle events",
"author": [
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Gold",
"given_name": "R. E.",
"clpid": "Gold-R-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "M\u00f6bius",
"given_name": "E.",
"clpid": "M\u00f6bius-E"
},
{
"family_name": "Popecki",
"given_name": "M.",
"clpid": "Popecki-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "We report studies of two large solar energetic particle (SEP) events on Nov. 4 and 6, 1997 that were observed using advanced energetic particle detectors on the ACE and the Wind spacecraft. Both events showed enriched Fe/O, and had a \u223c1 MeV/n ^3He/^4He ratio = 2.1 \u00d7 10^(\u22123), 4 times the coronal value. The Nov. 6 event had exceptionally hard spectra, with much higher intensities of high energy (10s of MeV) particles than the Nov. 4 event, yet below 1 MeV/n the intensities in the Nov. 6 event were lower than for Nov. 4. Strong, complex temporal variations observed for \u223c120 keV Fe/O contrasted with only gradual changes of this ratio at \u223c25 MeV/n. A spectral break was observed in the Nov. 6 event, wherein below a few MeV/n the spectra became harder. Taken together, these observations point to different seed and acceleration mechanisms dominating at low and high energies in these events.",
"doi": "10.1029/1998GL900235",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1999-01-15",
"series_number": "2",
"volume": "26",
"issue": "2",
"pages": "141-144"
},
{
"id": "authors:knhg2-9x340",
"collection": "authors",
"collection_id": "knhg2-9x340",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-113048212",
"type": "article",
"title": "Unusual isotopic composition of solar energetic particles observed in the November 6, 1997 event",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Dougherty",
"given_name": "B. L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Using the Solar Isotope Spectrometer on the Advanced Composition Explorer, we have measured the isotopic composition of solar energetic particles (SEPs) with energies of tens of MeV/nucleon during the November 6, 1997 solar event, including isotopes never before reported in SEPs, such as ^(34)S, ^(38)Ar, ^(44)Ca, ^(54)Fe, and ^(60)Ni, as well as isotopes of C, N, O, Ne, Mg, and Si. Abundances are found to be enhanced by factors of \u223c2 relative to the standard solar system values for ^(22)Ne/^(20)Ne and ^(26)Mg/^(24)Mg. Overall, the enrichments of the isotope ratios show a correlation with the ratio of masses, M_2/M_1, scaling approximately as (M_2/M_1)^7, although significant deviations from this trend are evident.",
"doi": "10.1029/1998GL900173",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1999-01-15",
"series_number": "2",
"volume": "26",
"issue": "2",
"pages": "153-156"
},
{
"id": "authors:z1hce-b0m16",
"collection": "authors",
"collection_id": "z1hce-b0m16",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-114427003",
"type": "article",
"title": "Inferred charge states of high energy solar particles from the Solar Isotope Spectrometer on ACE",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Dougherty",
"given_name": "B. L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The large solar event on November 6, 1997, was enriched in heavy elements (Fe/O \u223c 1) with very hard energy spectra (power law index of \u22122). There was also a large enrichment in heavier isotopes, suggesting unusually strong charge to mass (Q/M) fractionation (\u223c(Q/M)^(\u22127)). Assuming that the fractionation is dominated by Q/M and first ionization potential (FIP) related processes, we have inferred the charge states of twelve elements with energies of 12\u201360 MeV/nucleon. These results suggest a source temperature of 3\u20136 \u00d7 10^6K, significantly higher than deduced at lower energies.",
"doi": "10.1029/1998GL900218",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1999-01-15",
"series_number": "2",
"volume": "26",
"issue": "2",
"pages": "149-152"
},
{
"id": "authors:vx5eh-15c76",
"collection": "authors",
"collection_id": "vx5eh-15c76",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150213-093733570",
"type": "book_section",
"title": "The Time Delay between Nucleosynthesis and Acceleration Based on ACE Measurements of Primary Electron-Capture Nuclides",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "Supernovae should produce the radioactive nuclide ^(59)Ni, and in the ejecta of the explosions these particles will decay by electron capture with a halflife of 7.6 x 10^5 yr to produce ^(59)Co. However, if the ^(59)Ni nuclei are accelerated to cosmic-ray energies on a time scale short compared to this halflife, they are stripped of their electrons and decay is prevented. Thus the abundances of ^(59)Ni and ^(59)Co can be used to determine whether the time between nucleosynthesis and cosmic-ray acceleration is\nshort or long compared to the 59Ni halflife (Soutoul, Casse, & Juliusson 1978). We have used the Cosmic Ray Isotope Spectrometer (CRIS) on the Advanced Composition Explorer (ACE) to measure the abundances of 59Ni and 59Co in galactic cosmic rays, and find that the data are consistent with complete decay of 59Ni indicating a time delay 2 10^5 yr. We present the observations and discuss\ntheir significance for models of cosmic ray origin and acceleration.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:mct6w-e4a97",
"collection": "authors",
"collection_id": "mct6w-e4a97",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150212-115444336",
"type": "book_section",
"title": "Time Variations of Galactic Comic Ray Intensities Near Earth: 1997 to 1999",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "The time dependences of the intensities of low-energy galactic cosmic ray (GCR) nuclei have been investigated using instrumentation carried aboard the Advanced Composition Explorer (ACE). The intensities of these low energy particles near Earth began to decline from solar minimum levels in late-1997 /early-1998, shortly after the launch of ACE, and have been continuously monitored by the\nCosmic Ray Isotope Spectrometer (CRIS) instrument since that time. We find that the variations are well correlated with variations of higher energy cosmic rays, as indicated by neutron monitor observations. The relative magnitude of the GCR variations is significantly less than previously\nreported for anomalous cosmic rays. We also compare the fluctuations observed for different energies and different nuclides.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:48349-02z70",
"collection": "authors",
"collection_id": "48349-02z70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-114545256",
"type": "book_section",
"title": "Characteristics of 3He-Rich Energetic Particle Events Observed with the SIS Instrument on ACE",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We report observations of ^3He-rich solar energetic particle (SEP) events made with the Solar Isotope Spectrometer (SIS) aboard the Advanced Composition Explorer (ACE) spacecraft. SIS has been measuring helium isotopes above ~ 4 MeV /nucleon since August 1997 using a dE/dx vs. totalenergy\nsensor system employing large-area silicon solid-state detectors. We show examples of the helium isotope data being collected by SIS. Using data such as these it is possible to characterize the properties of ^3He-rich events including isotopic abundances, intensities, spectral hardness, and timing characteristics. These data can be correlated with other sources of information for the same events including particle measurements made at lower energies and observations of electromagnetic radiations from the flare site. Results of these types of analyses will be presented at the conference.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:p4cpx-h3277",
"collection": "authors",
"collection_id": "p4cpx-h3277",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150212-105955417",
"type": "book_section",
"title": "Long-Term Temporal Behavior of Interplanetary and Trapped Anomalous Cosmic Rays",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "New measurements of the long-term temporal history of anomalous cosmic rays (ACRs) at 1\nAU are presented, based on data from SAMPEX and ACE. Over the period from 1992 to 1997 the\ninterplanetary intensity of 8 to 27 MeV/nuc ACR oxygen increased by a factor of -5 as solar\nminimum approached. The intensity of ACR oxygen trapped in the Earth's magnetosphere\nshowed a corresponding time history. Early in 1998 both the interplanetary and trapped intensities\nsuddenly decreased with the onset of solar activity leading to the next solar maximum. We discuss\nthe relation of the time-delay between changes in the interplanetary and trapped fluxes, possible\nsolar/interplanetary causes of these changes, and the lifetime of trapped ACRs in Earth's\nmagnetosphere.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:p5wr8-srd21",
"collection": "authors",
"collection_id": "p5wr8-srd21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-163448873",
"type": "book_section",
"title": "Trans-Nickel Elements in Solar Energetic Particles",
"author": [
{
"family_name": "Sollitt",
"given_name": "L. S.",
"clpid": "Sollitt-L-S"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "The trans-nickel elements (Z \u2265 29) are some of the rarest in the Solar System; they typically are about\n1/1OOOth to l/lOOOOth as abundant as iron (Z = 26). We present measurements of zinc and other transnickel\nelements in solar energetic particle (SEP) events observed by the Solar Isotope Spectrometer (SIS) in\nthe energy range of 10-75 MeV/nuc. SIS is part of the Advanced Composition Explorer (ACE) spacecraft,\npresently in orbit about the Earth-Sun Ll point. The measured abundances of the trans-nickel elements are\ncompared to tabulated meteoritic and photospheric abundances and to previous SEP measurements. The results\nmay help to assess changes in composition due to SEP acceleration and transport.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:4kthd-h8326",
"collection": "authors",
"collection_id": "4kthd-h8326",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150212-163034160",
"type": "book_section",
"title": "Measurements of the Elemental Composition of Galactic Cosmic Ray Nuclei with 6\u2264Z\u226428 from the Cosmic Ray Isotope Spectrometer on ACE",
"author": [
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mahan",
"given_name": "S. E.",
"clpid": "Mahan-S-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "The elemental abundances of galactic cosmic rays (GCR) observed near Earth provide information about the\ncomposition of the cosmic ray sources as well as their propagation history. The Cosmic Ray Isotope Spectrometer\n(CRIS) onboard the Advanced Composition Explorer (ACE) spacecraft measures the elemental and isotopic composition of GCRs with energies '\"\" 50 - 500 Me V /nucleon with high statistical accuracy ('\"\" 5000 stopping nuclei heavier than helium per day) due to its large geometrical factor. The CRIS data are used to derive cosmic ray abundances at the lowest level of solar activity during the last solar minimum. We present elemental abundances measured by CRIS, compare them with previous measurements, and discuss the plausible origins of the disagreement.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:ybtrk-q4713",
"collection": "authors",
"collection_id": "ybtrk-q4713",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150213-094618167",
"type": "book_section",
"title": "Implications for Cosmic Ray Propagation from ACE Measurements of Radioactive Clock Isotope Abundances",
"author": [
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "Galactic cosmic rays (GCR) interact to produce secondary fragments as they pass through the interstellar medium (ISM). Abundances of the long-lived radioactive secondaries ^(10)Be, ^(26)Al, ^(36)Cl, and ^(54)Mn can be used to a derive the confinement time of cosmic rays in the galaxy. Abundances for these species have been measured recently using the Cosmic Ray Isotope Spectrometer (CRIS) aboard the Advanced Composition Explorer (ACE) spacecraft. To interpret this data we have modeled the production and propagation of the radioactive secondaries, taking into account recently published isotopic production cross-sections. Abundances for all species are consistent with a confinement time of \u03c0_(esc) ~22 x 10^6 years.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:phqca-7bs54",
"collection": "authors",
"collection_id": "phqca-7bs54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150212-113747616",
"type": "book_section",
"title": "Observations of the Solar Modulation of Galactic and Anomalous Cosmic Rays During Solar Minimum",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Blake",
"given_name": "J. B.",
"clpid": "Blake-J-B"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Hamilton",
"given_name": "D. C.",
"clpid": "Hamilton-D-C"
},
{
"family_name": "Hill",
"given_name": "M. E.",
"orcid": "0000-0002-5674-4936",
"clpid": "Hill-M-E"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Keppller",
"given_name": "E.",
"clpid": "Keppller-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Looper",
"given_name": "M. D.",
"clpid": "Looper-M-D"
},
{
"family_name": "Marsden",
"given_name": "R. G.",
"clpid": "Marsden-R-G"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Sanderson",
"given_name": "T. R.",
"clpid": "Sanderson-T-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N.",
"clpid": "Yanasak-N"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "From the end of 1997 to early 1998, the relatively steady-state solar-minimum conditions provided an ideal\nperiod to study the solar modulation of anomalous cosmic rays (ACRs) and galactic cosmic rays (GCRs).\nUsing observations of the energy spectra of the most abundant elements (H, He, C, N, 0, and Ne) from an\narray of spacecraft and instruments, we calculate the radial gradients for ACRs and GCRs over a wide range of\nrigidity. The GCR radial gradient is near zero for all rigidities, out to 70 AU. The ACR radial gradient shows\na strong rigidity dependence in the middle heliosphere, which is expected, but the rigidity dependence is not\npresent in the outer heliosphere, and is not obvious in the inner heliosphere.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:jq5vd-bhv16",
"collection": "authors",
"collection_id": "jq5vd-bhv16",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-090354763",
"type": "book_section",
"title": "A Tilt Model for Anomalous Cosmic Rays and the Location of the Solar Wind Termination Shock",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We use the observed relationship of the radial gradient of anomalous cosmic rays (ACRs), as measured in the outer heliosphere with instruments on the Voyager and Pioneer spacecraft, and the tilt of the heliospheric neutral current sheet to develop a model for the time dependence of ACRs at all radii near the helioequatorial plane. This phenomenological model reproduces the observations at 1 AU, Voyagers 1 and 2, and Pioneer 10 quite well. The model also indicates that the helioequatorial source intensity at the shock varies by a factor of 10, depending on solar magnetic polarity. The location of the solar wind termination shock during 1980-1990 is found to be 92 AU, with a best-fit of 84 AU.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:yav94-yj128",
"collection": "authors",
"collection_id": "yav94-yj128",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150212-103610912",
"type": "book_section",
"title": "Measurements of the Isotopic Composition of Anomalous Cosmic Ray N, O, and Ne from ACE",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We have measured the elemental and isotopic composition of anomalous cosmic rays (ACRs) with energies > 8 Me V /nucleon during solar quiet periods between August 1997 and March 1998, using the Solar Isotope Spectrometer (SIS) on the Advanced Composition Explorer (ACE). The capabilities of the SIS instrument allow the examination of spectra of individual ACR isotopes. In addition to the well-known low-energy ACR\nenhancements in the intensity of elemental 0 and Ne, similar enhancements are found in ^(18)O and ^(22)Ne, with\nrelative abundances of ^(18)O/^(16)O ~ 0.002 and ^(22)Ne/(20)Ne ~ 0.1. The neon abundance ratio appears more\nsimilar to that found in the solar wind than in meteorites, and is far below that deduced for the galactic cosmic\nray (GCR) source, indicating that GCRs are not simply an accelerated sample of the local interstellar medium.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:4y9z5-h1g45",
"collection": "authors",
"collection_id": "4y9z5-h1g45",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-084408358",
"type": "book_section",
"title": "Radial Interplanetary Mean Free Paths Inferred from Anomalous Cosmic Ray Observations in the Outer Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We use two independent techniques to estimate the rigidity dependence of the interplanetary mean free pathlength in the outer heliosphere in 1998: I) inferences from gradients of anomalous cosmic rays (ACRs) between Voyagers 1 and 2 and 2) inferences from the shape of the ACR energy spectra. Both techniques indicate that the mean free path increases rapidly between \"\"0.25 GV and I GV but is independent of rigidity above \"'J GV, in agreement with the dependence used by Steenberg et al. (I 999) to fit the 1998 ACR energy spectra using a full-drift, two-dimensional solution to the transport equation. The gradient method also yields an\nestimate of the magnitude of the mean free path, which is \"'2 \u00b1 0.4 AU at 1.5 GV, the same as the value of 2.0 AU used by Steenberg et al. (1999). In addition, we find that the mean free path at 0.42 GV is 1.4 \u00b1 0.8 from anisotropy measurements of 4-7.8 MeV/nuc ACR He from Voyager 1. This value is consistent with the estimate from the gradient method and from the Steenberg et al. fits. At 1.5 GV, the mean free path during the 1998 solar minimum is \"'I 0 times larger than that estimated for solar maximum in 1990, suggesting that for A>O, when particles drift from high to low latitudes, the radial gradient at low latitudes reflects the much\nsmaller radial gradients theoretically expected (Zank et al. 1998) at higher latitudes.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:0czpr-hqe36",
"collection": "authors",
"collection_id": "0czpr-hqe36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-103123111",
"type": "book_section",
"title": "Particle Acceleration and Sources in the November 1997 Solar Energetic Particle Events",
"author": [
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dwyer",
"given_name": "J. R.",
"clpid": "Dwyer-J-R"
},
{
"family_name": "Gold",
"given_name": "R. E.",
"clpid": "Gold-R-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "M\u00f6bius",
"given_name": "E.",
"clpid": "M\u00f6bius-E"
},
{
"family_name": "Popecki",
"given_name": "M.",
"clpid": "Popecki-M"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We repon studies of two large solar energetic panicle (SEP) events on Nov. 4 and 6. 1997 that were observed using advanced energetic panicle detectori; on the ACE and the Wind spacecraft. Both events showed enriched Fe/O, and had a ~1MeV/n ^3He/^4He ratio = 2.1x 10^(-3) , 4 times the coronal value. The Nov. 6 event had exceptionally hard spectra. with much higher intensities of high energy (10s of MeV) particles than the Nov. 4 event, yet below 1MeV per nucleon the intensities in the Nov. 6 event were lower than for\nNov. 4. Strong, complex temporal variations observed for ~120 keV Fe/0 contrasted with only gradual changes of this ratio at ~25 MeV/n. A spectural break was observed in the Nov. 6 event. wherein below a few MeV/n the spectra became harder. Taken together these observations point to different seed and acceleration mechanisms dominating at low and high energies in these events.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:agh84-pa702",
"collection": "authors",
"collection_id": "agh84-pa702",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-093110762",
"type": "book_section",
"title": "Composition of Anomalous Cosmic Rays and Other Ions from Voyager Observations",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Steenberg",
"given_name": "C. D.",
"clpid": "Steenberg-C-D"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We present energy spectra of eleven cosmic ray elements with energies from rv5 to rv500 MeV/nuc using data\nobtained from the Voyager spacecraft in the outer heliosphere from early 1993 to the end of 1998. The lowenergy intensity increases observed in all these spectra are consistent with the shapes expected to be exhibited\nby primarily singly-charged anomalous cosmic rays (ACRs). One of these elements is Na, which is being reported as a member of the ACR component for the first time. We find that the intensity increase below rv 10 Me V /nuc in the Si spectrum in the outer heliosphere is not dominated by re-accelerated solar wind. There is also evidence for a non-ACR component in the energy spectra of Mg, Si, and S observed at 1 AU by the Wind spacecraft below rv5 MeV/nuc. We see evidence in the energy spectra of Ar in both the inner and outer heliosphere for multiply-charged ACRs above rv360 MeV. Using a fit to the ACR intensities with a full-drift, two-dimensional numerical model of the acceleration and propagation of singly-charged ACRs, we present a table of the relative abundances of the seed particles of eleven elements at the solar wind termination shock.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:sj0f6-k1g47",
"collection": "authors",
"collection_id": "sj0f6-k1g47",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-142207624",
"type": "book_section",
"title": "Time Variations of Solar Energetic Particle Abundances Observed by the ACE Spacecraft",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"abstract": "The abundances of elements from Helium to Iron have been observed in nine different solar energetic particle (SEP) events using the Solar Isotope Spectrometer (SIS) on-board the Advanced Composition Explorer (ACE). SIS has a large geometry factor (~38 cm^2-sr), enabling us to observe abundances on a time scale of hours. In this paper we repo1t on substantial temporal variations of the observed abundances within events and from event to event. We wish to understand these results in terms of acceleration and\ntranspo1t processes, taking into account factors such as first ionization potential, particle charge states,\nspectral shape, and event type (gradual and impulsive). It is essential that these variations be understood if\nwe are to reliably estimate the composition of the sun from direct observations of SEP abundances.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:2ff39-79792",
"collection": "authors",
"collection_id": "2ff39-79792",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150206-150809671",
"type": "book_section",
"title": "A Study of ^3He Spectra and Abundances in Impulsive Solar Energetic Particle Events - Results from Measurements with ACE/SEPICA, ACE/SIS and SOHO/HSTOF",
"author": [
{
"family_name": "Bogdanov",
"given_name": "A. T.",
"clpid": "Bogdanov-A-T"
},
{
"family_name": "M\u00f6bius",
"given_name": "E.",
"clpid": "M\u00f6bius-E"
},
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Hilchenback",
"given_name": "M.",
"clpid": "Hilchenback-M"
},
{
"family_name": "Hovestadt",
"given_name": "D.",
"clpid": "Hovestadt-D"
},
{
"family_name": "Kistler",
"given_name": "L. M.",
"clpid": "Kistler-L-M"
},
{
"family_name": "Popecki",
"given_name": "M. A.",
"clpid": "Popecki-M-A"
},
{
"family_name": "Lund",
"given_name": "E. J.",
"clpid": "Lund-E-J"
},
{
"family_name": "Heirtzler",
"given_name": "D.",
"clpid": "Heirtzler-D"
},
{
"family_name": "Galvin",
"given_name": "A. B.",
"orcid": "0000-0003-3752-5700",
"clpid": "Galvin-A-B"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "Energy spectra of the He isotopes and the energy dependence of the ^3He/^4He ratio during a number of impulsive solar energetic particle events (SEP) observed between September 1997 and December 1998 are analyzed. Data covering the energy range from 0.1 to 10 MeV/amu were supplied by three instruments with complementary energy ranges: the Solar Energetic Particle Ionic Charge Analyzer (SEPICA) and the Solar Isotope Spectrometer (SIS) on ACE, and the time-of-flight mass spectrometer HSTOF on SOHO. We confirm the trend of a monotonic increase of the 3He abundance with energy up to a maximum in the region of a few MeV/amu found in previous ISEE studies and extend the analysis to events of intermediate 3He enrichment. We briefly discuss the observational data and their relation to existing theoretical work on selection and acceleration mechanisms in impulsive flares.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:vcq9w-whc32",
"collection": "authors",
"collection_id": "vcq9w-whc32",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150213-105040374",
"type": "book_section",
"title": "Time Variations of the Modulation of Anomalous and Galactic Cosmic Rays",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "Between the launch of the Advanced Composition Explorer (ACE) in 1997 and the end of 1999, the intensities of galactic cosmic rays at 1 AU have dropped almost a factor of 2, and the anomalous cosmic rays have decreased by an even larger amount. The large collecting power of the Cosmic Ray Isotope Spectrometer (CRIS) and the Solar Isotope Spectrometer (SIS) instruments on ACE allow us to investigate the changing modulation on short time scales and at different rigidities. Using anomalous cosmic ray (ACR) and galactic cosmic ray (OCR) intensities of He,\nC, O, Ne, Si, S, and Fe, and energies from ~ 6 MeV/nucleon to ~ 460 MeV/nucleon, we examine the differences between the short term and long term effects. We observe the expected correlation of these intensities with neutron\nmonitor data, but see little correlation of OCR and ACR intensities with the locally measured magnetic field.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:ezv0v-95471",
"collection": "authors",
"collection_id": "ezv0v-95471",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150212-094216395",
"type": "book_section",
"title": "Measurements of the Heavy-Ion Isotopic Composition of Solar Energetic Particles",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "Using the Solar Isotope Spectrometer (SIS) on the Advanced Composition Explorer (ACE) spacecraft, we have measured the isotopic composition of ten elements from C to Ni (Z = 6 to 28) at energies of tens of MeV/nucleon in as many as nine solar energetic particle (SEP) events that have occurred since November 1997. We find that the isotopic composition varies dramatically from event to event. For example, the ^(22)Ne/^(20)Ne ratio ranges from ~0.7 to 2 times the solar wind value. The mass fractionation is strongly correlated with the Fe/O and other element abundance ratios, suggesting that the elemental and isotopic fractionation are governed by the same process.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:77vpk-4r192",
"collection": "authors",
"collection_id": "77vpk-4r192",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150210-162025599",
"type": "book_section",
"title": "Measurements of the Isotopic Abundances of Galactic Cosmic Rays and Their Implications for Cosmic Ray Origin",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.L.",
"clpid": "Lijowski-M-L"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Ramaty",
"given_name": "Reuven",
"clpid": "Ramaty-R"
},
{
"family_name": "Vangioni-Flam",
"given_name": "Elisabeth",
"clpid": "Vangion-Flam-E"
},
{
"family_name": "Cass\u00e9",
"given_name": "Michel-",
"clpid": "Cass\u00e9-M"
},
{
"family_name": "Olive",
"given_name": "Keith",
"clpid": "Olive-K"
}
],
"abstract": "We present measurements of the nickel and cobalt isotopes\nfrom the Cosmic Ray Isotope Spectrometer (CRJS) which was launched in\nAugust, 1997 aboard the NASA Advanced Composition Explorer (ACE).\nThe objectives of CRJS are to measure the isotopic abundances and energy\nspectra of galactic cosmic rays ~GCRs) with 3 \u2264 Z \u2264 30. We find\nthat for these nuclei the measured ^5Ni/^(60)Ni and ^(59)Co/^(60)Ni ratios imply\na time delay between nucleosynthesis and acceleration to cosmic ray\nenergies of > 10^5 y.",
"publisher": "Astronomical Society of the Pacific",
"publication_date": "1999"
},
{
"id": "authors:dk81c-bt866",
"collection": "authors",
"collection_id": "dk81c-bt866",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140226-111247648",
"type": "article",
"title": "Anomalous cosmic rays: Observations",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "The latitudinal gradients of galactic cosmic ray protons and anomalous cosmic ray (ACR) helium appear to be symmetrical about a plane displaced \u223c10\u00b0 south of the heliographic equator, similar to the displacement of the heliospheric current sheet (HCS). The radial gradient of \u223c10 MeV/nuc ACR oxygen in the outer heliosphere is correlated with the amplitude of the tilt of the HCS. The form of the correlation depends on the magnetic polarity of the solar cycle. The observed radial gradients are the basis for an empirical model that reasonably describes the modulation of \u223c2\u20133 GV ACR oxygen at low heliographic latitudes over a 25-year period.",
"doi": "10.1016/S0273-1177(99)80005-2",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "1999",
"series_number": "3",
"volume": "23",
"issue": "3",
"pages": "509-520"
},
{
"id": "authors:d6mht-rbg39",
"collection": "authors",
"collection_id": "d6mht-rbg39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-164947365",
"type": "book_section",
"title": "Correlated Elemental and Isotopic Variations in Solar Energetic Particles",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We consider whether the observed fractionation of Ne isotopes recently reported in solar energetic particle\n(SEP) events is due to the same charge-to-mass dependent fractionation processes that apparently cause SEP elemental composition variations. We find that the observed correlation of the 22Ne/20Ne and Na/Mg ratios in nine large SEP events is consistent with a common fractionation process if the charge states of these ions are characteristic of a source temperature of -1.5 to -4 million degrees.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:7bg5j-k1c15",
"collection": "authors",
"collection_id": "7bg5j-k1c15",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-145949528",
"type": "book_section",
"title": "New Measurements of Solar Particle Events Enriched in Heavy Ions",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "The four most heavy-ion-rich of the nine largest solar energetic particle events detected by the Solar Isotope Spectrometer on the ACE, are the focus of this paper. We have used isotopic measurements of Ne to determine the degree of charge/mass fractionation and infer the charge states of C - Ni in these events. The results indicate a source temperature of ~ 4 x 10^6 K; this and the measured abundances suggest that these four events more similar to impulsive events than gradual. Although the ^3He/^4He ratios are not enhanced to the level typical of impulsive events, there are measurable enhancements over typical solar wind values in three of the events.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:7fnm1-zy753",
"collection": "authors",
"collection_id": "7fnm1-zy753",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150213-092825276",
"type": "book_section",
"title": "Cosmic Ray Source Abundances for 29\u2264Z\u226434",
"author": [
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "The Cosmic Ray Isotope Spectrometer (CRIS) instrument on board the Advanced Composition Explorer (ACE) spacecraft is making new measurements of nuclides just beyond the iron-nickel peak in the galactic cosmic rays. Isotopes of copper and zinc have been resolved for the first time. Elemental abundances for nuclei with 29\u2264Z\u226434 are reported with good separation between species. Several of these elements are useful for studying fractionation processes which may depend on the first ionization potential or volatility. Source abundances are estimated using a prior propagation calculation and their potential for distinguishing between source models are discussed.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:wesmb-av949",
"collection": "authors",
"collection_id": "wesmb-av949",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-091921800",
"type": "book_section",
"title": "Drift Calculations on the Modulation of Anomalous Cosmic Rays During the 1998 Solar Minimum Period",
"author": [
{
"family_name": "Steenberg",
"given_name": "C. D.",
"clpid": "Steenberg-C-D"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We present full-drift solutions of the two-dimensional cosmic ray transport equation in an ongoing study to explain ACR observations made in the outer heliosphere. Calculated spectra are compared to 1998 ACR H, He, 0, N, and Ne observations from Voyager I and 2. It is found that the modulation is dominated by diffusion at the spacecraft positions and that the spectra of all the above species can be reasonably explained using a single set of modulation parameters. These include diffusion mean free paths with a magnitude significantly smaller at the shock than at the spacecraft positions.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:wcpfn-fwd38",
"collection": "authors",
"collection_id": "wcpfn-fwd38",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150212-102928289",
"type": "book_section",
"title": "Measurements of the Elemental Composition and Energy Spectra of Anomalous Cosmic Ray Nuclei by the Solar Isotopic Spectrometer on ACE",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Sollitt",
"given_name": "L. S.",
"clpid": "Sollitt-L-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "The Solar Isotope Spectrometer (SIS) instrument on the Advanced Composition Explorer (ACE) spacecraft provides high resolution measurements of the elemental and isotopic compositions of energetic nuclei between approximately 10 and 100 Me V /nucleon from He to Zn (Z = 2 to 30). Solar quiet times from late 1997 to the present will be used to measure the energy spectra of elements previously observed in the anomalous cosmic rays, as well as search for new, rare elements. Relative abundances of the observed species will also be derived and related to the abundances of neutral atoms in the local interstellar medium.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:kw6nf-zq891",
"collection": "authors",
"collection_id": "kw6nf-zq891",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150212-102026660",
"type": "book_section",
"title": "Measurements of ^3He and Heavy Elements in Impulsive SEP Events",
"author": [
{
"family_name": "Slocum",
"given_name": "P. L.",
"clpid": "Slocum-P-L"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "The Solar Isotope Spectrometer (SIS), an instrument on board the Advanced Composition Explorer (ACE), measures solar energetic particle (SEP) elemental and isotopic abundances during solar events. During solar quiet times, SIS measures isotopes of low-energy cosmic rays from the Galaxy and isotopes of the anomalous cosmic ray component. The heavy element content at ~10-20 MeV /nuc of two SEP events with large enhancements (>400x) of the ^3He/^4He ratio relative to coronal composition has been studied. We find heavy element abundance ratios which are consistent with those derived from past studies of ^3He-rich events within statistical limitations.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:afsva-fd028",
"collection": "authors",
"collection_id": "afsva-fd028",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150213-100300982",
"type": "book_section",
"title": "Secondary Electron-Capture Clock Isotopes as a Probe of Reacceleration",
"author": [
{
"family_name": "Mahan",
"given_name": "S.E.",
"clpid": "Mahan-S-E"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "Cosmic rays that are produced by nuclear interactions during propagation and decay only by electron capture can be used to determine the level of cosmic ray reacceleration that has occurred. The high resolution, large statistical sample of cosmic rays collected by the Cosmic Ray Isotope Spectrometer (CRIS) aboard the Advanced Composition Explorer (ACE) spacecraft provides a data set that allows precision measurements of these isotopic abundances. We discuss electron capture decay, the signatures of\nreacceleration, and the sensitivity with which reacceleration models can be tested.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:zedfy-5c850",
"collection": "authors",
"collection_id": "zedfy-5c850",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150213-095550927",
"type": "book_section",
"title": "Radioactive Clock Isotope Abundance Measurements from the CRIS Experiment aboard the ACE Spacecraft",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Yanasak",
"given_name": "N. E.",
"clpid": "Yanasak-N-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "George",
"given_name": "J. S.",
"clpid": "George-J-S"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Lijowski",
"given_name": "M.",
"clpid": "Lijowski-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "Radioactive cosmic ray nuclei produced by nuclear interactions during cosmic ray propagation through the galaxy can be used to study the mean interstellar gas density in the propagation volume and the time scales associated with the propagation process. The Cosmic Ray Isotope Spectrometer (CRIS) aboard the Advanced Composition Explorer (ACE) has made high-resolution abundance measurements of the beta-decay secondary isotopes ^(10)Be, ^(26)Al, ^(36)Cl, and ^(54)Mn over the energy range 70-400 MeV/nuc. The large geometrical factor of CRIS (~250 cm^2sr) and the 20 months of data collection at near solar minimum conditions have made it possible since launch in August, 1997 to accumulate data samples considerably larger than previous missions. The isotopic abundances derived from these data are presented and compared with previous measurements.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:43h9y-mhr41",
"collection": "authors",
"collection_id": "43h9y-mhr41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-091234906",
"type": "book_section",
"title": "Voyager Observations of Anomalous and Galactic Cosmic Rays During 1998",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Hamilton",
"given_name": "D. C.",
"clpid": "Hamilton-D-C"
},
{
"family_name": "Hillard",
"given_name": "M. E.",
"clpid": "Hillard-M-E"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
}
],
"contributor": [
{
"family_name": "Kieda",
"given_name": "D.",
"clpid": "Kieda-D"
},
{
"family_name": "Salamon",
"given_name": "M.",
"clpid": "Salamon-M"
},
{
"family_name": "Dingus",
"given_name": "B.",
"clpid": "Dingus-B"
}
],
"abstract": "We present energy spectra of anomalous and galactic cosmic rays over a wide energy range by combining data from the Low Energy Charged Particle experiment and the Cosmic Ray experiment on the Voyager spacecraft. The data set covers all of 1998. We compare energy spectra obtained from Voyagers 1 and 2. The energy range covered contains the peak intensity in the spectra for anomalous cosmic ray hydrogen, helium, and oxygen. The spectra presented can be used to constrain models of solar modulation.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1999"
},
{
"id": "authors:ynxp5-kej13",
"collection": "authors",
"collection_id": "ynxp5-kej13",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131031-083104716",
"type": "article",
"title": "The Cosmic-Ray Isotope Spectrometer for the Advanced Composition Explorer",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Gauld",
"given_name": "B.",
"clpid": "Gauld-B"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Thayer",
"given_name": "M. R.",
"clpid": "Thayer-M-R"
}
],
"abstract": "The Cosmic-Ray Isotope Spectrometer is designed to cover the highest decade of the Advanced Composition Explorer's energy interval, from \u223c50 to \u223c500 MeV nucl^(\u22121), with isotopic resolution for elements from Z\u22432 to Z\u224330. The nuclei detected in this energy interval are predominantly cosmic rays originating in our Galaxy. This sample of galactic matter can be used to investigate the nucleosynthesis of the parent material, as well as fractionation, acceleration, and transport processes that these particles undergo in the Galaxy and in the interplanetary medium.\nCharge and mass identification with CRIS is based on multiple measurements of dE/dx and total energy in stacks of silicon detectors, and trajectory measurements in a scintillating optical fiber trajectory (SOFT) hodoscope. The instrument has a geometrical factor of \u223cr250 cm^2 sr for isotope measurements, and should accumulate \u223c5\u00d710^6 stopping heavy nuclei (Z>2) in two years of data collection under solar minimum conditions.",
"doi": "10.1023/A:1005075813033",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "1998-07",
"series_number": "1-4",
"volume": "86",
"issue": "1-4",
"pages": "285-356"
},
{
"id": "authors:9hyf7-f8e28",
"collection": "authors",
"collection_id": "9hyf7-f8e28",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160406-113935658",
"type": "article",
"title": "Global Processes that Determine Cosmic Ray Modulation",
"author": [
{
"family_name": "Fisk",
"given_name": "L. A.",
"clpid": "Fisk-L-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "The global processes that determine cosmic ray modulation are reviewed. The essential elements of the theory which describes cosmic ray behavior in the heliosphere are summarized, and a series of discussions is presented which compare the expectations of this theory with observations of the spatial and temporal behavior of both galactic cosmic rays and the anomalous component; the behavior of cosmic ray electrons and ions; and the 26-day variations in cosmic rays as a function of heliographic latitude. The general conclusion is that the current theory is essentially correct. There is clear evidence, in solar minimum conditions, that the cosmic rays and the anomalous component behave as is expected from theory, with strong effects of gradient and curvature drifts. There is strong evidence of considerable latitude transport of the cosmic rays, at all energies, but the mechanism by which this occurs is unclear. Despite the apparent success of the theory, there is no single choice for the parameters which describe cosmic ray behavior, which can account for all of the observed temporal and spatial variations, spectra, and electron vs. ion behavior.",
"doi": "10.1023/A:1005074923940",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "1998-01",
"series_number": "1-2",
"volume": "83",
"issue": "1-2",
"pages": "179-214"
},
{
"id": "authors:ntx1g-crn67",
"collection": "authors",
"collection_id": "ntx1g-crn67",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140908-101152277",
"type": "article",
"title": "Anomalous cosmic rays and solar modulation",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "We review aspects of anomalous cosmic rays (ACRs) that bear on the solar modulation of energetic particles in the heliosphere. We show that the latitudinal and radial gradients of these particles exhibit a 22-year periodicity in concert with the reversal of the Sun's magnetic field. The power-law index of the low energy portion of the energy spectrum of ACRs at the shock in 1996 appears to be \u2264 -1.3, suggesting that the strength of the solar wind termination shock at the helioequatorial plane is relatively weak, with s \u2264 2.8. The rigidity dependence of the perpendicular interplanetary mean free path in the outer heliosphere for particles with rigidities between \u223c 0.2 and 0.7 GV varies approximately as R^2, where R is particle rigidity. There is evidence that ACR oxygen is primarily multiply charged above \u223c 20 MeV/nuc and primarily singly-charged below \u223c 16 MeV/nuc. The location of the termination shock was at \u223c 65 AU in 1987 and \u223c 85 AU in 1994.",
"doi": "10.1023/A:1005027929871",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "1998-01",
"series_number": "1-2",
"volume": "83",
"issue": "1-2",
"pages": "357-408"
},
{
"id": "authors:a7edy-g7851",
"collection": "authors",
"collection_id": "a7edy-g7851",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140908-101236271",
"type": "article",
"title": "The solar isotope spectrometer for the Advanced Composition Explorer",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Gauld",
"given_name": "B.",
"clpid": "Gauld-B"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Thayer",
"given_name": "M. R.",
"clpid": "Thayer-M-R"
},
{
"family_name": "Dougherty",
"given_name": "B. L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Grumm",
"given_name": "R. L.",
"clpid": "Grumm-R-L"
},
{
"family_name": "Milliken",
"given_name": "B. D.",
"clpid": "Milliken-B-D"
},
{
"family_name": "Radocinski",
"given_name": "R. G.",
"clpid": "Radocinski-R-G"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Shuman",
"given_name": "S.",
"clpid": "Shuman-S"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The Solar Isotope Spectrometer (SIS), one of nine instruments on the Advanced Composition Explorer (ACE), is designed to provide high- resolution measurements of the isotopic composition of energetic nuclei from He to Zn (Z=2 to 30) over the energy range from \u223c10 to \u223c100 MeV nucl^(\u22121). During large solar events SIS will measure the isotopic abundances of solar energetic particles to determine directly the composition of the solar corona and to study particle acceleration processes. During solar quiet times SIS will measure the isotopes of low-energy cosmic rays from the Galaxy and isotopes of the anomalous cosmic-ray component, which originates in the nearby interstellar medium. SIS has two telescopes composed of silicon solid-state detectors that provide measurements of the nuclear charge, mass, and kinetic energy of incident nuclei. Within each telescope, particle trajectories are measured with a pair of two-dimensional silicon-strip detectors instrumented with custom, very large-scale integrated (VLSI) electronics to provide both position and energy-loss measurements. SIS was especially designed to achieve excellent mass resolution under the extreme, high flux conditions encountered in large solar particle events. It provides a geometry factor of \u223c40 cm^2 sr, significantly greater than earlier solar particle isotope spectrometers. A microprocessor controls the instrument operation, sorts events into prioritized buffers on the basis of their charge, range, angle of incidence, and quality of trajectory determination, and formats data for readout by the spacecraft. This paper describes the design and operation of SIS and the scientific objectives that the instrument will address.",
"doi": "10.1023/A:1005027929871",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "1998",
"series_number": "1-4",
"volume": "86",
"issue": "1-4",
"pages": "357-408"
},
{
"id": "authors:4xm08-gte56",
"collection": "authors",
"collection_id": "4xm08-gte56",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141203-160500797",
"type": "book_section",
"title": "Implications of 26-Day Variations for the Global Modulation",
"book_title": "Cosmic Rays in the Heliosphere",
"author": [
{
"family_name": "Zhang",
"given_name": "M.",
"clpid": "Zhang-M"
},
{
"family_name": "Simpson",
"given_name": "J. A.",
"clpid": "Simpson-J-A"
},
{
"family_name": "Kunow",
"given_name": "H.",
"clpid": "Kunow-H"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
},
{
"family_name": "Burger",
"given_name": "R.A.",
"clpid": "Burger-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"contributor": [
{
"family_name": "Fisk",
"given_name": "L. A.",
"clpid": "Fisk-L-A"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Simnett",
"given_name": "G. M.",
"clpid": "Simnett-G-M"
},
{
"family_name": "von Steiger",
"given_name": "R.",
"clpid": "von-Steiger-R"
},
{
"family_name": "Wenzel",
"given_name": "K.-P.",
"clpid": "Wenzel-K-P"
}
],
"doi": "10.1007/978-94-017-1189-0",
"isbn": "978-90-481-5032-8",
"publisher": "Springer",
"place_of_publication": "Dordrecht, Netherlands",
"publication_date": "1998",
"pages": "203-207"
},
{
"id": "authors:yhnv6-egt46",
"collection": "authors",
"collection_id": "yhnv6-egt46",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150107-155451895",
"type": "book_section",
"title": "Anomalous Cosmic Rays",
"book_title": "Cosmic Rays in the Heliosphere",
"author": [
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"contributor": [
{
"family_name": "Fisk",
"given_name": "Lennard A.",
"clpid": "Fisk-L-A"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Simnett",
"given_name": "G. M.",
"clpid": "Simnett-G-M"
},
{
"family_name": "von Steiger",
"given_name": "R.",
"clpid": "von-Steiger-R"
},
{
"family_name": "Wenzel",
"given_name": "K.-P.",
"clpid": "Wenzel-K-P"
}
],
"abstract": "We review the observed properties of anomalous cosmic rays and the present status of our knowledge of the processes by which they originate. We compiled a comprehensive set of ACR energy spectral data from various spacecraft throughout the heliosphere during the passes of Ulysses over the poles of the Sun and present first results of a detailed modeling effort. In several contributions, we discuss the questions of injection and possible pre-acceleration of pickup ions, summarize new observations on the ionic charge composition, and present new results on the composition of minor ions in ACRs.",
"doi": "10.1007/978-94-017-1189-0_18",
"isbn": "978-90-481-5032-8",
"publisher": "Springer",
"place_of_publication": "Dordrecht, Netherlands",
"publication_date": "1998",
"pages": "259-308"
},
{
"id": "authors:aa4f1-18547",
"collection": "authors",
"collection_id": "aa4f1-18547",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150108-163318431",
"type": "article",
"title": "Anomalous Cosmic Ray Data Sets",
"author": [
{
"family_name": "Marsden",
"given_name": "R. G.",
"clpid": "Marsden-R-G"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Lanzerotti",
"given_name": "L. J.",
"clpid": "Lanzerotti-L-J"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "McKibben",
"given_name": "R. B.",
"clpid": "McKibben-R-B"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Trattner",
"given_name": "K. J.",
"clpid": "Trattner-K-J"
}
],
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "1998",
"pages": "263-269"
},
{
"id": "authors:en7kj-e1t09",
"collection": "authors",
"collection_id": "en7kj-e1t09",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-225449871",
"type": "book_section",
"title": "Intensity Gradients of Anomalous Cosmic Ray Oxygen Throughout the Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Marsden",
"given_name": "R. G.",
"clpid": "Marsden-R-G"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Reames",
"given_name": "D. V.",
"clpid": "Reames-D-V"
},
{
"family_name": "Trattner",
"given_name": "K.J.",
"clpid": "Trattner-K-J"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
},
{
"family_name": "Raubenheimer",
"given_name": "C.",
"clpid": "Raubenheimer-C"
},
{
"family_name": "van der Walt",
"given_name": "D. J.",
"clpid": "van-der-Walt-D-J"
}
],
"abstract": "We use anomalous cosmic ray oxygen energy spectra collected from five different locations in the\nheliosphere during three time periods to estimate the radial and latitudinal gradients of the particle\nintensities at three energies. The three periods include the two high-latitude passes of Ulysses over\nthe solar poles and the last few months of the cosmic ray oxygen data from Pioneer 10. The radial\ngradient is modeled as a power law in radius and the latitudinal gradient is assumed to be constant.\nThe gradients are analyzed in two ways: the first uses the actual average spacecraft latitudes and the\nsecond assumes the symmetry plane of the heliosphere is at 10\u00b0 S in heliolatitude. Reasonable fits\nare obtained under either assumption concerning the location of the symmetry plane, although the\nlatitudinal gradients are smaller by a factor of~ 2 if the symmetry plane is offset by l0\u00b0 S. The radial\ngradient exhibits a radial dependence of ~r^(-1) or r^(-2) depending on whether the symmetry plane is the\nhelioequator or not, respectively. The r^(-2) dependence is not consistent with the gradient measured\nin a similar part of the solar cycle ~20 years ago, suggesting that the helioequator is the likely plane\nof symmetry for these particles. The only significant difference in oxygen flux between polar passes\noccurs at < 10 Me V /nuc and is similar to that observed one year earlier in the outer heliosphere due\nto decreasing solar modulation.",
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1997"
},
{
"id": "authors:b6pmy-dxt74",
"collection": "authors",
"collection_id": "b6pmy-dxt74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141022-160308145",
"type": "book_section",
"title": "The ACE-CRIS Scintillating Optical Fiber Trajectory (SOFT) Detector: Calibrations at the NSCL and GSI",
"author": [
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Allbritton",
"given_name": "G.",
"clpid": "Allbritton-G"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dougherty",
"given_name": "B. L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Dowkonnt",
"given_name": "P. F.",
"clpid": "Dowkonnt-P-F"
},
{
"family_name": "Epstein",
"given_name": "J. W.",
"clpid": "Epstein-J-W"
},
{
"family_name": "Fridovich",
"given_name": "B.",
"clpid": "Fridovich-B"
},
{
"family_name": "Gauld",
"given_name": "B.",
"clpid": "Gauld-B"
},
{
"family_name": "Grumm",
"given_name": "R.",
"clpid": "Grumm-R"
},
{
"family_name": "Hink",
"given_name": "P. L.",
"clpid": "Hink-P-L"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Madden",
"given_name": "M. P.",
"clpid": "Madden-M-P"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Milliken",
"given_name": "B.",
"clpid": "Milliken-B"
},
{
"family_name": "Olevitch",
"given_name": "M. A.",
"clpid": "Olevitch-M-A"
},
{
"family_name": "Radocinski",
"given_name": "R. G.",
"clpid": "Radocinski-R-G"
},
{
"family_name": "Shuman",
"given_name": "S.",
"clpid": "Shuman-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Thayer",
"given_name": "M. R.",
"clpid": "Thayer-M-R"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
},
{
"family_name": "Raubenheimer",
"given_name": "C.",
"clpid": "Raubenheimer-C"
},
{
"family_name": "van der Walt",
"given_name": "D. J.",
"clpid": "van-der-Walt-D-J"
}
],
"abstract": "The Scintillating Optical Fiber Trajectory (SOFT) detector, the hodoscope for the Cosmic Ray Isotope Spectrometer (CRIS) on the NASA Advanced Composition Explorer, was calibrated using 155 MeV/n He, Li, C, N, 0, and Ar at the Michigan State University National Superconducting\nCyclotron Laboratory (NSCL), and 200 - 700 MeV/n C, Si, and Fe at the GSI facility in Darrnstadt. Germany. The flight instrument consists of three hodoscope fiber planes and one trigger plane. read out by an image intensified CCD camera system and by intensified photodiodes respectively. The\nspatial and angular resolution of the hodoscope is described, along with the detection efficiency of both the hodoscope and trigger plane as a function of charge.",
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1997"
},
{
"id": "authors:zghw6-yg338",
"collection": "authors",
"collection_id": "zghw6-yg338",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-225735470",
"type": "book_section",
"title": "Rigidity Dependence of the Interplanetary Mean Free Path",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"abstract": "We use energy spectra of anomalous cosmic rays derived from data from experiments on the Voyager\nand Pioneer spacecraft to inf er the rigidity dependence of the perpendicular interplanetary mean free\npath over the rigidity range ~0.3 to 4 GV. Data are from three intervals: 1993/157-209, 1994/157-\n313, and l 996/1-52. We use two techniques to estimate that the rigidity dependence is approximately\nproportional to R^2 at low rigidities with a flattening above ~1 GV, roughly consistent with recent\ntheoretical estimates (Bieber et al. 1995).",
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1997"
},
{
"id": "authors:nt6nf-7b957",
"collection": "authors",
"collection_id": "nt6nf-7b957",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141022-105048424",
"type": "book_section",
"title": "Silicon Strip Detectors with Custom VLSI Readout Electronics for the SIS Instrument of ACE",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dougherty",
"given_name": "B. L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Gauld",
"given_name": "B.",
"clpid": "Gauld-B"
},
{
"family_name": "Grumm",
"given_name": "R.",
"clpid": "Grumm-R"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Kleinfelder",
"given_name": "S.A.",
"clpid": "Kleinfelder-S-A"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Radocinski",
"given_name": "R. G.",
"clpid": "Radocinski-R-G"
},
{
"family_name": "Shuman",
"given_name": "S.",
"clpid": "Shuman-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Thayer",
"given_name": "M. R.",
"clpid": "Thayer-M-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
},
{
"family_name": "van der Walt",
"given_name": "D. J.",
"clpid": "van-der-Walt-D-J"
},
{
"family_name": "Raubenheimer",
"given_name": "C.",
"clpid": "Raubenheimer-C"
}
],
"abstract": "We discuss the design and implementation of the trajectory system for the Solar Isotope Spectrometer (SIS) instrument on the Advanced Composition Explorer (ACE) mission. Thin, large area silicon strip detectors instrumented with a custom very large scale integrated circuit (VLSI) pulse height analyzer (PHA) for each strip are used to simultaneously achieve large geometrical factor and the capability for making precise measurements in even the largest solar energetic particle (SEP) events.",
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1997"
},
{
"id": "authors:f70kd-22x45",
"collection": "authors",
"collection_id": "f70kd-22x45",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-225253772",
"type": "book_section",
"title": "Evolution of the Energy Spectra of Anomalous Cosmic Rays in the Outer Heliosphere",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
},
{
"family_name": "Raubenheimer",
"given_name": "C.",
"clpid": "Raubenheimer-C"
},
{
"family_name": "van der Walt",
"given_name": "D. J.",
"clpid": "van-der-Walt-D-J"
}
],
"abstract": "We present energy spectra of anomalous cosmic ray hydrogen, helium, and oxygen derived from data\ncollected from experiments on the Voyager and Pioneer spacecraft from 1993 through 1996. The sequence\nof energy spectra show the effects of decreasing modulation as the solar cycle approaches and\nreaches solar minimum conditions. We suggest a number of factors that may be responsible for the\nspectral evolution, including the approach of the spacecraft to the source region of the particles (the\nsolar wind termination shock), possible changes in the source strength, decreasing tilt of the neutral\ncurrent sheet, and changes in the diffusion mean free path. We find that the data are inconsistent with\nsource strength changes, but changes due to the other factors are possible and will require more complete\n2 and 3-dimensional propagation models to make quantitative assessments. We find evidence\nfor anomalous cosmic ray hydrogen up to energies as high as 400 MeV/nuc.",
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1997"
},
{
"id": "authors:rrm9x-fht69",
"collection": "authors",
"collection_id": "rrm9x-fht69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-224734935",
"type": "book_section",
"title": "Evidence for Anomalous Cosmic Ray S, Si, and Fe in the Outer Heliosphere and for A Non-ACR Source of S at 1 AU",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"contributor": [
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
},
{
"family_name": "Raubenheimer",
"given_name": "C.",
"clpid": "Raubenheimer-C"
},
{
"family_name": "van der Walt",
"given_name": "D. J.",
"clpid": "van-der-Walt-D-J"
}
],
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1997"
},
{
"id": "authors:k4mbe-sjj25",
"collection": "authors",
"collection_id": "k4mbe-sjj25",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-225100732",
"type": "book_section",
"title": "Updated Measurements of the Isotopic Composition of Interplanetary and Geomagnetically Trapped Anomalous Cosmic Rays",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
},
{
"family_name": "Raubenheimer",
"given_name": "C.",
"clpid": "Raubenheimer-C"
},
{
"family_name": "van der Walt",
"given_name": "D. J.",
"clpid": "van-der-Walt-D-J"
}
],
"abstract": "Pure samples of anomalous cosmic rays are measured by SAMP EX, both at latitudes where the geomagnetic\nfield acts as a particle rigidity filter, and in the radiation belt of trapped anomalous cosmic\nrays. We report updated measurements of the isotopic composition of anomalous cosmic ray N, 0,\nand Ne in these two regions, along with isotopic values measured over the poles, and compare our\nresults with those found by previous investigators and with those measured in other samples of solar\nand galactic material.",
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1997"
},
{
"id": "authors:5tbg3-a4572",
"collection": "authors",
"collection_id": "5tbg3-a4572",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141022-100159601",
"type": "book_section",
"title": "Large-Area Silicon Detectors for the Advanced Composition Explorer (ACE) Solar Isotope Spectrometer (SIS)",
"author": [
{
"family_name": "Dougherty",
"given_name": "B. L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Allbritton",
"given_name": "G.L.",
"clpid": "Allbriton-G-L"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Gauld",
"given_name": "B.",
"clpid": "Gauld-B"
},
{
"family_name": "Grumm",
"given_name": "R.",
"clpid": "Grumm-R"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Madden",
"given_name": "M.",
"clpid": "Madden-M"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Milliken",
"given_name": "B.",
"clpid": "Milliken-B"
},
{
"family_name": "Radocinski",
"given_name": "R. G.",
"clpid": "Radocinski-R-G"
},
{
"family_name": "Sears",
"given_name": "B.",
"clpid": "Sears-B"
},
{
"family_name": "Shuman",
"given_name": "S.",
"clpid": "Shuman-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Thayer",
"given_name": "M. R.",
"clpid": "Thayer-M-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
},
{
"family_name": "Raubenheimer",
"given_name": "C.",
"clpid": "Raubenheimer-C"
},
{
"family_name": "van der Walt",
"given_name": "D. J.",
"clpid": "van-der-Walt-D-J"
}
],
"abstract": "Extensive measurements were made of the thicknesses and dead-layers of the large-area, highpurity silicon detectors used for the Solar Isotope Spectrometer (SIS), an instrument to be launched on the Advanced Composition Explorer (ACE) spacecraft. Tests using accelerated beams of heavy nuclei were also carried out to characterize the completed instrument.",
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1997"
},
{
"id": "authors:n3azy-84130",
"collection": "authors",
"collection_id": "n3azy-84130",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-220904845",
"type": "book_section",
"title": "Two-Dimensional Position-Sensitive Silicon Detectors For The ACE Solar Isotope Spectrometer",
"book_title": "Gamma-Ray and Cosmic-Ray Detectors, Techniques, and Missions",
"author": [
{
"family_name": "Wiedenbeck",
"given_name": "Mark E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Christian",
"given_name": "Eric R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cook",
"given_name": "Walter R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dougherty",
"given_name": "Brian L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Leske",
"given_name": "Richard A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "Edward C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "Tycho T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Ramsey",
"given_name": "Brian D.",
"clpid": "Ramsey-B-D"
},
{
"family_name": "Parnell",
"given_name": "Thomas A.",
"clpid": "Parnell-T-A"
}
],
"abstract": "Two-dimensional position-sensitive silicon detectors ('matrix detectors') have been designed, procured, and tested as part of the development of the solar isotope spectrometer (SIS) instrument for NASA's Advanced Composition Explorer (ACE) mission. Important characteristics of these devices include: thickness approximately 50 - 90 micrometer, active area 34 cm^2, 64 strips on each surface with 1 mm strip pitch. The SIS instrument uses four such detectors, processing signals from each of the 512 individual strips with a separate 12-bit pulse height analyzer implemented with custom-designed VLSI circuits. A set of 25 matrix detectors have been characterized through a variety of tests intended both toe select the best candidates for use in the flight instrument and to provide the calibrations needed to interpret flight data. We discuss the design of the SIS matrix detectors and present selected results from the detector tests that have been performed.",
"doi": "10.1117/12.253977",
"isbn": "9780819421944",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "1996-10-18",
"pages": "176-187"
},
{
"id": "authors:72kv3-jah68",
"collection": "authors",
"collection_id": "72kv3-jah68",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-215930019",
"type": "book_section",
"title": "Characterization Of Large-Area Silicon Ionization Detectors For The ACE Mission",
"book_title": "Gamma-Ray and Cosmic-Ray Detectors, Techniques, and Missions",
"author": [
{
"family_name": "Dougherty",
"given_name": "Brian L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Christian",
"given_name": "Eric R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "Richard A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Milliken",
"given_name": "Barrett D.",
"clpid": "Milliken-B-D"
},
{
"family_name": "von Rosenvinge",
"given_name": "Tycho T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "Mark E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Ramsey",
"given_name": "Brian D.",
"clpid": "Ramsey-B-D"
},
{
"family_name": "Parnell",
"given_name": "Thomas A.",
"clpid": "Parnell-T-A"
}
],
"abstract": "We report on extensive tests of large-area (10 cm diameter) high-purity ion-implanted silicon detectors for the solar isotope spectrometer (SIS), and lithium-drifted silicon detectors for the cosmic ray isotope spectrometer (CRIS), which are under development for launch on the advanced composition explorer (ACE) mission. Depletion and breakdown characteristics versus bias were studied, as were long-term current and noise stability in a thermally cycled vacuum. Dead-layer and total thickness maps were obtained using laser interferometry, beams of energetic argon nuclei and radioactive sources of alpha particles. Results, selection criteria, and yields are presented.",
"doi": "10.1117/12.253978",
"isbn": "9780819421944",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "1996-10-18",
"pages": "188-198"
},
{
"id": "authors:3n9dw-xvh63",
"collection": "authors",
"collection_id": "3n9dw-xvh63",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-215730302",
"type": "article",
"title": "The Isotopic Composition of Anomalous Cosmic Rays from SAMPEX",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Measurements of the anomalous cosmic ray (ACR) isotopic composition have been made in three regions of the magnetosphere accessible from the polar Earth orbit of SAMPEX, including the interplanetary medium at high latitudes and geomagnetically trapped ACRs. At those latitudes where ACRs can penetrate the Earth's magnetic field while fully stripped galactic cosmic rays (GCRs) of similar energies are excluded, a pure ACR sample is observed to have the following composition: ^(15)N/N < 0.023, ^(18)O/^(16)O < 0.0034, and ^(22)Ne/^(20)Ne = 0.077(+0.085, -0.023). We compare our values with those found by previous investigators and with those measured in other samples of solar and galactic material. In particular, a comparison of ^(22)Ne/^(20)Ne measurements from various sources implies that GCRs are not simply an accelerated sample of the local interstellar medium.",
"doi": "10.1007/BF00170801",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "1996-10",
"series_number": "1-2",
"volume": "78",
"issue": "1-2",
"pages": "149-154"
},
{
"id": "authors:ydbyt-b3s41",
"collection": "authors",
"collection_id": "ydbyt-b3s41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-214818330",
"type": "article",
"title": "Composition of Anomalous Cosmic Rays and Implications for the Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "We use energy spectra of anomalous cosmic rays (ACRs) measured with the Cosmic Ray instrument on the Voyager 1 and 2 spacecraft during the period 1994/157-313 to determine several parameters of interest to heliospheric studies. We estimate that the strength of the solar wind termination shock is 2.42 (-0.08, +0.04). We determine the composition of ACRs by estimating their differential energy spectra at the shock and find the following abundance ratios: H/He = 5.6 (-0.5, +0.6), C/He = 0.00048 \u00b1 0.00011, N/He = 0.011 \u00b1 0.001, O/He = 0.075 \u00b1 0.006, and Ne/He = 0.0050 \u00b1 0.0004. We correlate our observations with those of pickup ions to deduce that the long-term ionization rate of neutral nitrogen at 1 AU is ~8.3 \u00d7 10^(-7) s^(-1) and that the charge-exchange cross section for neutral N and solar wind protons is ~1.0 \u00d7 10^(-15) cm^2 at 1.1 keV. We estimate that the neutral C/He ratio in the outer heliosphere is 1.8(-0.7, +0.9) \u00d7 10^(-5). We also find that heavy ions are preferentially injected into the acceleration process at the termination shock.",
"doi": "10.1007/BF00170798",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "1996-10",
"series_number": "1-2",
"volume": "78",
"issue": "1-2",
"pages": "117-128"
},
{
"id": "authors:ks654-asn52",
"collection": "authors",
"collection_id": "ks654-asn52",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-220236671",
"type": "article",
"title": "Ionization Processes in the Heliosphere - Rates and Methods of their Determination",
"author": [
{
"family_name": "Ruci\u0144ski",
"given_name": "D.",
"clpid": "Ruci\u0144ski-D"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Gloeckler",
"given_name": "G.",
"clpid": "Gloeckler-G"
},
{
"family_name": "Lazarus",
"given_name": "A. J.",
"clpid": "Lazarus-A-J"
},
{
"family_name": "M\u00f6bius",
"given_name": "E.",
"clpid": "M\u00f6bius-E"
},
{
"family_name": "Witte",
"given_name": "M.",
"clpid": "Witte-M"
}
],
"abstract": "The rates of the most important ionization processes acting in interplanetary space on interstellar H, He, C, O, Ne and Ar atoms are critically reviewed in the paper. Their long-term modulations in the period 1974 \u2013 1994 are reexamined using updated information on relevant cross-sections as well as direct or indirect data on variations of the solar wind/solar EUV fluxes based on IMP 8 measurements and monitoring of the solar 10.7 cm radio emission. It is shown that solar cycle related variations are pronounced (factor of \u223c 3 between maximum and minimum) especially for species such as He, Ne, C for which photoionization is the dominant loss process. Species sensitive primarily to the charge-exchange (as H) show only moderate fluctuations \u223c 20% around average. It is also demonstrated that new techniques that make use of simultaneous observations of neutral He atoms on direct and indirect orbits, or simultaneous measurements of He^+ and He^(++) pickup ions and solar wind particles can be useful tools for narrowing the uncertainties of the He photoionization rate caused by insufficient knowledge of the solar EUV flux and its variations.",
"doi": "10.1007/BF00170794",
"issn": "0038-6308",
"publisher": "Springer",
"publication": "Space Science Reviews",
"publication_date": "1996-10",
"series_number": "1-2",
"volume": "78",
"issue": "1-2",
"pages": "73-76"
},
{
"id": "authors:kkm3c-te598",
"collection": "authors",
"collection_id": "kkm3c-te598",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-214349007",
"type": "article",
"title": "Evidence for Multiply Charged Anomalous Cosmic Rays",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "New measurements from the SAMPEX spacecraft show that most anomalous cosmic ray (ACR) oxygen nuclei with energies above 20 MeV nucleon^(-1) are multiply ionized, with ionic charge states of Q = 2, Q = 3, and probably higher. This new result contrasts with lower energies, at which most ACRs are singly charged. The observed abundance of multiply charged ions agrees with estimates of the fraction of singly charged ACRs that undergo electron stripping during acceleration if the timescale for acceleration to 10 MeV nucleon^(-1) is ~1 yr. The existence of multiply charged ACRs helps explain their acceleration to high energies, and it has implications for several other studies.",
"doi": "10.1086/310169",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "1996-07-20",
"series_number": "1",
"volume": "466",
"issue": "1",
"pages": "L43-L46"
},
{
"id": "authors:2vg49-n8b06",
"collection": "authors",
"collection_id": "2vg49-n8b06",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140612-105003970",
"type": "article",
"title": "The Distance to the Solar Wind Termination Shock in 1993 and 1994 from Observations of Anomalous Cosmic Rays",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "Using data from the Voyager and Pioneer spacecraft, we examine the energy spectra of anomalous cosmic rays (ACRs) during 1992\u20131994, a period of rapidly increasing intensities of these particles in the outer heliosphere. The 1992 period appears to be in nonequilibrium, marked by a rapid decrease in the tilt of the current sheet from \u223c63\u00b0 to \u223c35\u00b0 and a complex, evolving magnetic topology that affects interplanetary drifts and drift acceleration along the solar wind termination shock. In addition, large propagating interplanetary disturbances in 1991 may have weakened the shock temporarily, reducing the intensity of accelerated ions. The 1993\u20131994 period appears to be in quasi-equilibrium, marked by a stable tilt of the current sheet and a steady, large-scale magnetic topology that provides stable conditions for propagation and acceleration. The ACR intensities of higher-rigidity particles rise slowly during this period, suggesting that the shock intensity has stabilized. At lower rigidities the ACR intensities are increasing rapidly, which we attribute to decreasing modulation. During 1994 days 157\u2013209, we estimate that the shock was at 85 \u00b1 5 AU. The shock strength s is estimated to be 2.63 \u00b1 0.14, significantly weaker than a strong shock (s = 4) and consistent with a termination shock modified by the pressure of galactic cosmic rays. By comparing these 1994 observations with those made in 1987, we estimate that the latitudinal gradient of ACR He with energies 31\u201357 MeV nucleon^(\u22121) is \u223c1.9%/deg along the shock from the equator to the pole. We estimate that the ratio of the efficiency of injection of He^+ to H^+ pickup ions into the acceleration process is 7.0 \u00b1 1.6.",
"doi": "10.1029/96JA00413",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1996-05",
"series_number": "A5",
"volume": "101",
"issue": "A5",
"pages": "11017-11025"
},
{
"id": "authors:fgd37-awd11",
"collection": "authors",
"collection_id": "fgd37-awd11",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140624-140158949",
"type": "article",
"title": "A Study of the Composition and Energy Spectra of Anomalous Cosmic Rays Using the Geomagnetic Field",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "We use instrumentation on SAMPEX and the Earth's field as a magnetic rigidity filter in a \"double spectrometer\" approach to measure the composition and energy spectra of anomalous cosmic rays (ACRs) with Z\u22656. A \"pure\" sample of anomalous cosmic ray C, N, O, and Ne is obtained, with no significant evidence for other species. The bulk of ACRs are now known to be singly-charged, and the geomagnetic filter allows their energy spectra to be measured to higher energies than before. The anomalous oxygen spectrum is found to extend to at least \u223c100 MeV/nuc, which has implications for models of the acceleration of these ions.",
"doi": "10.1029/96GL00423",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1996-03-15",
"series_number": "6",
"volume": "23",
"issue": "6",
"pages": "617-620"
},
{
"id": "authors:mkkb2-zd876",
"collection": "authors",
"collection_id": "mkkb2-zd876",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200511-145902680",
"type": "book_section",
"title": "Composition of Anomalous Cosmic Rays and Implications for the Heliosphere",
"book_title": "The Heliosphere in the Local Interstellar Medium",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "von Steiger",
"given_name": "R.",
"clpid": "von-Steiger-R"
},
{
"family_name": "Lallement",
"given_name": "R.",
"clpid": "Lallement-R"
},
{
"family_name": "Lee",
"given_name": "M. A.",
"clpid": "Lee-Martin-A"
}
],
"abstract": "We use energy spectra of anomalous cosmic rays (ACRs) measured with the Cosmic Ray instrument on the Voyager 1 and 2 spacecraft during the period 1994/157-313 to determine several parameters of interest to heliospheric studies. We estimate that the strength of the solar wind termination shock is 2.42 (-0.08, +0.04). We determine the composition of ACRs by estimating their differential energy spectra at the shock and find the following abundance ratios: H/He = 5.6 (-0.5, +0.6), C/He = 0.00048 \u00b1 0.00011, N/He = 0.011 \u00b1 0.001, O/He = 0.075 \u00b1 0.006, and Ne/He = 0.0050 \u00b1 0.0004. We correlate our observations with those of pickup ions to deduce that the long-term ionization rate of neutral nitrogen at 1 AU is ~8.3 \u00d7 10\u207b\u2077 s\u207b\u00b9 and that the charge-exchange cross section for neutral N and solar wind protons is ~1.0 \u00d7 10\u207b\u00b9\u2075 cm\u00b2 at 1.1 keV. We estimate that the neutral C/He ratio in the outer heliosphere is 1.8(-0.7, +0.9) \u00d7 10\u207b\u2075. We also find that heavy ions are preferentially injected into the acceleration process at the termination shock.",
"doi": "10.1007/978-94-009-1782-8_13",
"isbn": "978-94-010-7296-0",
"publisher": "Springer Netherlands",
"place_of_publication": "Dordrecht",
"publication_date": "1996",
"pages": "117-128"
},
{
"id": "authors:ny774-x0h91",
"collection": "authors",
"collection_id": "ny774-x0h91",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200511-153142800",
"type": "book_section",
"title": "Ionization Processes in the Heliosphere \u2014 Rates and Methods of Their Determination",
"book_title": "The Heliosphere in the Local Interstellar Medium",
"author": [
{
"family_name": "Ruci\u0144ski",
"given_name": "D.",
"clpid": "Ruci\u0144ski-D"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Gloeckler",
"given_name": "G.",
"clpid": "Gloeckler-G"
},
{
"family_name": "Lazarus",
"given_name": "A. J.",
"clpid": "Lazarus-A-J"
},
{
"family_name": "M\u00f6bius",
"given_name": "E.",
"clpid": "M\u00f6bius-E"
},
{
"family_name": "Witte",
"given_name": "M.",
"clpid": "Witte-M"
}
],
"contributor": [
{
"family_name": "von Steiger",
"given_name": "R.",
"clpid": "von-Steiger-R"
},
{
"family_name": "Lallement",
"given_name": "R.",
"clpid": "Lallement-R"
},
{
"family_name": "Lee",
"given_name": "M. A.",
"clpid": "Lee-Martin-A"
}
],
"abstract": "The rates of the most important ionization processes acting in interplanetary space on interstellar H, He, C, O, Ne and Ar atoms are critically reviewed in the paper. Their long-term modulations in the period 1974 \u2013 1994 are reexamined using updated information on relevant cross-sections as well as direct or indirect data on variations of the solar wind/solar EUV fluxes based on IMP 8 measurements and monitoring of the solar 10.7 cm radio emission. It is shown that solar cycle related variations are pronounced (factor of \u223c 3 between maximum and minimum) especially for species such as He, Ne, C for which photoionization is the dominant loss process. Species sensitive primarily to the charge-exchange (as H) show only moderate fluctuations \u223c 20% around average. It is also demonstrated that new techniques that make use of simultaneous observations of neutral He atoms on direct and indirect orbits, or simultaneous measurements of He\u207a and He\u207a\u207a pickup ions and solar wind particles can be useful tools for narrowing the uncertainties of the He photoionization rate caused by insufficient knowledge of the solar EUV flux and its variations.",
"doi": "10.1007/978-94-009-1782-8_9",
"isbn": "9789401072960",
"publisher": "Springer Netherlands",
"place_of_publication": "Dordrecht",
"publication_date": "1996",
"pages": "73-84"
},
{
"id": "authors:9r0xx-btd81",
"collection": "authors",
"collection_id": "9r0xx-btd81",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140724-155533705",
"type": "book_section",
"title": "The Solar Isotope Spectrometer (SIS)",
"author": [
{
"family_name": "Cohen",
"given_name": "C. M. S.",
"orcid": "0000-0002-0978-8127",
"clpid": "Cohen-C-M-S"
},
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Dougherty",
"given_name": "Brian L.",
"clpid": "Dougherty-B-L"
},
{
"family_name": "Gauld",
"given_name": "B.",
"clpid": "Gauld-B"
},
{
"family_name": "Grumm",
"given_name": "R.",
"clpid": "Grumm-R"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Milliken",
"given_name": "B.",
"clpid": "Milliken-B"
},
{
"family_name": "Radocinski",
"given_name": "R. G.",
"clpid": "Radocinski-R-G"
},
{
"family_name": "Shuman",
"given_name": "S.",
"clpid": "Shuman-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Thayer",
"given_name": "M. R.",
"clpid": "Thayer-M-R"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Potgieter",
"given_name": "M. S.",
"clpid": "Potgieter-M-S"
}
],
"abstract": "The Solar Isotope Spectrometer (SIS) is scheduled for launch on NASA's Advanced Composition Explorer (ACE) mission. SIS has two solid-state telescopes that are designed to measure the elemental and isotopic composition of solar energetic particles and anomalous cosmic rays in the energy range from rv 10 to 100 Me V /nucleon, including elements from He to Zn (2\u2264Z\u226430). This paper presents\na brief description of the design and operation of SIS.",
"publisher": "Potchefstroom University, Space Research Unit",
"publication_date": "1996"
},
{
"id": "authors:m54xd-z8303",
"collection": "authors",
"collection_id": "m54xd-z8303",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141202-163530409",
"type": "book_section",
"title": "Past, Present, and Future Cosmic Ray Identification Applications for Large Area Silicon Detectors",
"author": [
{
"family_name": "Walton",
"given_name": "J. T.",
"clpid": "Walton-J-T"
},
{
"family_name": "Lee",
"given_name": "J. S.",
"clpid": "Lee-J-S"
},
{
"family_name": "Lewak",
"given_name": "D.",
"clpid": "Lewak-D"
},
{
"family_name": "Wong",
"given_name": "Y. K.",
"clpid": "Wong-Y-K"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
},
{
"family_name": "Knowlton",
"given_name": "W. B.",
"clpid": "Knowlton-W-B"
},
{
"family_name": "Haller",
"given_name": "E. E.",
"clpid": "Haller-E-E"
}
],
"abstract": "An overview of the application of Si(Li) detectors to cosmic-ray identification is presented. A vacancy-related defect in FZ silicon that can limit the lithium compensation process in Si(Li) detector fabrication is discussed and a gettering process to remove this defect\nis outlined. Computer simulation of the gettering process is shown to yield native point defect diffusivity and concentration values approaching those recently proposed by G\u00f6sele, Pl\u00f6\u03b2l and Tan.",
"publisher": "Electrochemical Society",
"publication_date": "1996"
},
{
"id": "authors:tch0e-4p194",
"collection": "authors",
"collection_id": "tch0e-4p194",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200511-151236312",
"type": "book_section",
"title": "The Isotopic Composition of Anomalous Cosmic Rays from Sampex",
"book_title": "The Heliosphere in the Local Interstellar Medium",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "von Steiger",
"given_name": "R.",
"clpid": "von-Steiger-R"
},
{
"family_name": "Lallement",
"given_name": "R.",
"clpid": "Lallement-R"
},
{
"family_name": "Lee",
"given_name": "M. A.",
"clpid": "Lee-Martin-A"
}
],
"abstract": "Measurements of the anomalous cosmic ray (ACR) isotopic composition have been made in three regions of the magnetosphere accessible from the polar Earth orbit of SAMPEX, including the interplanetary medium at high latitudes and geomagnetically trapped ACRs. At those latitudes where ACRs can penetrate the Earth's magnetic field while fully stripped galactic cosmic rays (GCRs) of similar energies are excluded, a pure ACR sample is observed to have the following composition: \u00b9\u2075N/N < 0.023, \u00b9\u2078O/\u00b9\u2076O < 0.0034, and \u00b2\u00b2Ne/\u00b2\u2070Ne = 0.077(+0.085, -0.023). We compare our values with those found by previous investigators and with those measured in other samples of solar and galactic material. In particular, a comparison of \u00b2\u00b2Ne/\u00b2\u2070Ne measurements from various sources implies that GCRs are not simply an accelerated sample of the local interstellar medium.",
"doi": "10.1007/978-94-009-1782-8_16",
"isbn": "9789401072960",
"publisher": "Springer Netherlands",
"place_of_publication": "Dordrecht",
"publication_date": "1996",
"pages": "149-154"
},
{
"id": "authors:58mnk-qaq43",
"collection": "authors",
"collection_id": "58mnk-qaq43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140219-110824481",
"type": "article",
"title": "Observations of Anomalous Cosmic-Ray Hydrogen from the Voyager Spacecraft",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "As Voyager 1 and 2 approach the solar wind termination shock, the hydrogen energy spectrum exhibits a\nrapidly increasing flux of anomalous cosmic-ray hydrogen, consistent with that observed for other anomalous\ncosmic-ray species. These results are consistent with the evidence for anomalous cosmic-ray hydrogen reported\nfrom Voyager observations during the period of minimum solar modulation in 1987.",
"doi": "10.1086/187941",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "1995-06-20",
"series_number": "2",
"volume": "446",
"issue": "2",
"pages": "L105-L108"
},
{
"id": "authors:58k5k-1cg32",
"collection": "authors",
"collection_id": "58k5k-1cg32",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140612-094752170",
"type": "article",
"title": "Anomalous Cosmic Ray Oxygen Gradients Throughout the Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Blake",
"given_name": "J. B.",
"clpid": "Blake-J-B"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Franz",
"given_name": "M.",
"clpid": "Franz-M"
},
{
"family_name": "Hovestadt",
"given_name": "D.",
"clpid": "Hovestadt-D"
},
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "We have used data from the Solar, Anomalous, and Magnetospheric Particle Explorer (SAMPEX), Ulysses, Voyager 1, Voyager 2, and Pioneer 10 spacecraft to determine the radial and latitudinal gradients of anomalous cosmic ray oxygen at 10 MeV/nuc during the last half of 1993. These five spacecraft cover radial distances from 1 AU (SAMPEX) to 58 AU (P10) and latitudes to 41 deg S (Ulysses) and 32 deg N (V1). We find that the radial gradient is a decreasing function of radial distance, approximately r-n, with n = 1.7 +/- 0.7. The large-scale radial gradient between the inner and outer heliosphere is much smaller than it was during the last solar minimum period in approximately 1987. The latitudinal gradient is small and positive, 1.3 +/- 0.4 %/deg, as opposed to the large and negative latitudinal gradients found during 1987, but similar to the small positive latitudinal gradient measured during 1976 for anomalous cosmic ray helium. These observations confirm that effects of curvature and gradient drift in the large scale magnetic field of the Sun are important for establishing the three-dimensional intensity distributions of these particles in the heliosphere during periods of solar minimum conditions",
"doi": "10.1029/94GL03343",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1995-02-15",
"series_number": "4",
"volume": "22",
"issue": "4",
"pages": "341-344"
},
{
"id": "authors:ttg4q-6am81",
"collection": "authors",
"collection_id": "ttg4q-6am81",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140616-163231974",
"type": "book_section",
"title": "Radial and Latitudinal Gradients of Anomalous Cosmic Ray Oxygen Throughout the Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Blake",
"given_name": "J. B.",
"clpid": "Blake-J-B"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Franz",
"given_name": "M.",
"clpid": "Franz-M"
},
{
"family_name": "Hovestadt",
"given_name": "D.",
"clpid": "Hovestadt-D"
},
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Iucci",
"given_name": "N.",
"clpid": "Iucci-N"
},
{
"family_name": "Lamanna",
"given_name": "E.",
"clpid": "Lamanna-E"
}
],
"abstract": "We have used data from the SAMPEX. Ulysses, Voyager 1 (Vl), Voyager\n2 (V2), and Pioneer 10 (PIO) spacecraft to determine the radial and latitudinal\ngradients of anomalous cosmic ray oxygen at 10 MeV/nuc during\n1994 days 209 - 313. These five spacecraft cover radial distances from 1\nAU (SAMPEX) to 61 AU (PIO) and latitudes to 80\u00b0 S (Ulysses) and 33\u00b0 N\n(Vl). We find that the radial gradient is a decreasing function of radial\ndistance, -r^(-n)\n, with n = 0.7 \u00b1 0.7. The large-scale radial gradient between\nthe inner and outer heliosphere is much smaller than it was during the last\nsolar minimum period in ~1987. The latitudinal gradient is small and\npositive, 2.1 \u00b1 0.6 %/deg, as opposed to the large and negative latitudinal\ngradients found during 1987, but similar to the small positive latitudinal\ngradient reported in a similar study for 1993 and also similar to that measured\nduring 1976 for anomalous cosmic ray helium. These observations\nconfirm that effects of curvature and gradient drift in the large scale magnetic\nfield of the Sun are important for establishing the three-dimensional\nintensity distributions of these particles in the heliosphere during periods of\nsolar minimum conditions.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1995"
},
{
"id": "authors:e67q2-3sf69",
"collection": "authors",
"collection_id": "e67q2-3sf69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140616-162118203",
"type": "book_section",
"title": "The Reappearance of Anomalous Cosmic Ray Hydrogen",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Iucci",
"given_name": "N.",
"clpid": "Iucci-N"
},
{
"family_name": "Lamanna",
"given_name": "E.",
"clpid": "Lamanna-E"
}
],
"abstract": "New observations from the Cosmic Ray Subsystem (CRS) on the Voyager\nspacecraft clearly show that anomalous cosmic ray hydrogen has reappeared,\nclearing up a controversy that has existed since the previous solar\nminimum [l, 2]. The new observations are consistent with the evidence for\nanomalous cosmic ray hydrogen seen in the 1987 solar minimum. Comparison\nof the anomalous and galactic cosmic ray modulation for the two\nsolar minima indicates that there is substantial modulation of the galactic\ncosmic rays beyond the solar wind termination shock.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1995"
},
{
"id": "authors:v1fbt-qvn73",
"collection": "authors",
"collection_id": "v1fbt-qvn73",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140616-163928405",
"type": "book_section",
"title": "Evolution of the Energy Spectra of Anomalous Cosmic Rays in the Outer Heliosphere and the Distance to the Solar Wind Termination Shock",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Iucci",
"given_name": "N.",
"clpid": "Iucci-N"
},
{
"family_name": "Lamanna",
"given_name": "E.",
"clpid": "Lamanna-E"
}
],
"abstract": "Using data from the Voyager 1 and 2 (Vl and V2) spacecraft, we examine\nthe energy spectra of anomalous cosmic rays (ACRs) for three time periods\nin 1993 - 1994. We use a spherically-symmetric model of the propagation\nof ACRs in the heliosphere to derive the energy spectrum of ACRs at the\nsolar wind termination shock and the shock's location. We find that in late\n1994 the shock strength has a value of 2.40 \u00b1 0.12 and is located at 84.2\n(-2.2, +2.6) AU.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1995"
},
{
"id": "authors:v05mc-je054",
"collection": "authors",
"collection_id": "v05mc-je054",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140612-134940854",
"type": "book_section",
"title": "Elemental Composition of the Anomalous Cosmic Ray Component",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Iucci",
"given_name": "N.",
"clpid": "Iucci-N"
},
{
"family_name": "Lamanna",
"given_name": "E.",
"clpid": "Lamanna-N"
}
],
"abstract": "We present a new determination of the abundances (normalized to He I and Ne I) of neutral atoms HI, CI, NI, 0I, and ArI in the very local interstellar medium. These abundances are derived from 1994 Voyager 1 observations of the energy spectra of the anomalous cosmic ray (ACR) component. We find that the abundances of NI, 0I, and ArI are in good agreement with solar system abundances, while the abundance of HI is -1/10 and that of CI is -1/80 of the solar system values, respectively. The low HI abundance suggests that H may be partially assimilated into the solar wind or is disfavored in the acceration process. The low CI abundance is\nconsistent with the expectation that C is mostly ionized in the local interstellar\nmedium. We find no evidence for significant charge-changing\ninteractions associated with the heliosheath region or with significant\ndepletion of atoms into grains in the very local interstellar medium.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1995"
},
{
"id": "authors:pwabj-rjd21",
"collection": "authors",
"collection_id": "pwabj-rjd21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140616-163700853",
"type": "book_section",
"title": "Radial and Latitudinal Gradients of Anomalous Cosmic Rays in the Outer Heliosphere",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Iucci",
"given_name": "N.",
"clpid": "Iucci-N"
},
{
"family_name": "Lamanna",
"given_name": "E.",
"clpid": "Lamanna-E"
}
],
"abstract": "We use recent data from the Voyager 1 and 2 and Pioneer 10 spacecraft to\ndetermine the radial and latitudinal gradients of anomalous cosmic rays\n(ACRs) in the outer heliosphere. The latitudinal gradient is small and\npositive, as opposed to the large and negative values observed during the\nlast solar minimum in 1987. The radial gradient is small and steady. We\ncompare our results with current theories of the acceleration and propagation\nof ACRs. We also suggest that the large increase in the intensity of\nACR helium that we observe during 1992 is due primarily to a change in \u00b7\nthe ACR source flux as interplanetary conditions approach quasi-equilibrium.\nThe continuing increases at lower energies in 1993 and 1994\nare consistent with a decreasing level of modulation during a period of\nquasi-equilibrium.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1995"
},
{
"id": "authors:h4ef9-2qn05",
"collection": "authors",
"collection_id": "h4ef9-2qn05",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140612-132930616",
"type": "article",
"title": "Observations of Anomalous Cosmic Rays in the Heliosphere from the SAMPEX, Ulysses, Voyager, and Pioneer Spacecraft",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Blake",
"given_name": "B.",
"clpid": "Blake-B"
},
{
"family_name": "Fr\u00e4enz",
"given_name": "M.",
"clpid": "Fr\u00e4enz-M"
},
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Hovestadt",
"given_name": "D.",
"clpid": "Hovestadt-D"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "The radial and latitudinal gradients of anomalous cosmic rays (ACRs) in the heliosphere are \nexpected to depend on the phase of the solar cycle. During the last solar minimum in 1987, when \npositive energetic particles were entering the heliosphere along the neutral current sheet, the \nradial gradient of these particles in the outer heliosphere was found to depend on the tilt of the \nsheet and was a minimum when the tilt assumed its minimum value. The latitudinal gradient was large \nand negative during this same period. On a large scale, the radial gradient from l to -40 AU was \nfound to decrease linearly with radial distance for ACR oxygen. These particle distributions are \nexpected to be different after the polarity reversal of the solar magnetic field, which occurred \n-1990. By July 1994, the Voyagers 1 and 2 (Vl and V2) and Pioneer 10 (PlO) spacecraft will be \npositioned in the outer heliosphere in the radial range 45 to 62 AU. V2 and PlO will be at \nrelatively low heliographic latitudes, while V l will be at 32\u00b0 N. In the inner heliosphere Ulysses \nwill be beyond 70\u00b0 S at a radial distance of 2.7 AU. The SAMPEX spacecraft is in a near-polar Earth \norbit. Using measurements of anomalous cosmic rays from instruments on these 5 spacecraft, we will \nreport on the temporal behavior of the fluxes and their radial and latitudinal gradients during the \ncurrent approach towards solar minimum. We will compare the results from those taken during the \nlast solar minimum period and relate these to current models of solar modulation.",
"doi": "10.1016/0273-1177(95)00357-K",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "1995",
"series_number": "9",
"volume": "16",
"issue": "9",
"pages": "337"
},
{
"id": "authors:zmsnk-p4f20",
"collection": "authors",
"collection_id": "zmsnk-p4f20",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140620-162104120",
"type": "article",
"title": "The Energy Spectra of Anomalous Cosmic Rays in the Outer Heliosphere During 1991-1994",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"abstract": "Since the launch of the Voyager spacecraft in 1977, we have monitored the energy spectra of anomalous cosmic rays (ACRs) as a function of radial and latitudinal position over the course of the solar cycle, including two reversals of the Sun's magnetic field. The energy spectrum for ACR helium observed during the last solar minimum period in 1987 at approximately 23 AU showed a rather narrow peak at approximately 22 MeV/nuc. In 1978 at approximately 2 AU, this spectrum was much broader with a peak at lower energies, in agreement with theories of the acceleration and propagation of these particles which include curvature and gradient drift in the interplanetary magnetic field. Currently, in the outer heliosphere at the position of Voyager 1 (approximately 55 AU and 32 deg N), the energy spectrum of ACR helium has a peak energy at approximately 8 MeV/nuc, considerably lower than previously observed. At Voyager 2 (42 AU and 11 deg S), the energy spectrum is quite different, having a peak energy near 20 MeV/nuc. We will report on the evolution of the spectra of ACRs as observed by the instruments on the Voyager spacecraft as the fluxes again approach solar minimum levels, expected in 1994, and relate the observations to models of their propagation.",
"doi": "10.1016/0273-1177(95)00370-T",
"issn": "0273-1177",
"publisher": "Elsevier",
"publication": "Advances in Space Research",
"publication_date": "1995",
"series_number": "9",
"volume": "16",
"issue": "9",
"pages": "363"
},
{
"id": "authors:6dgrm-rqt78",
"collection": "authors",
"collection_id": "6dgrm-rqt78",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140609-161515101",
"type": "book_section",
"title": "Two-Dimensional Interdigitated Pixel Detector for Energetic Particle Spectrometers",
"author": [
{
"family_name": "Cook",
"given_name": "Walter R., III",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Williams",
"given_name": "Daniel A.",
"clpid": "Williams-D-A"
},
{
"family_name": "Cunningham",
"given_name": "Thomas J.",
"clpid": "Cunningham-T-J"
},
{
"family_name": "Mazed",
"given_name": "Mohammad",
"clpid": "Mazed-M"
},
{
"family_name": "Fossum",
"given_name": "Eric R.",
"clpid": "Fossum-E-R"
}
],
"contributor": [
{
"family_name": "Cutts",
"given_name": "James A.",
"clpid": "Cutts-J-A"
}
],
"abstract": "This paper describes a type of cosmic ray detector suitable for the construction of a small, low power space-based instrument to detect the energy and isotope of energetic nuclei, such as those produced by solar flares. The detector is similar to previous types of silicon PIN detectors where the fully depleted body of the wafer comprises the intrinsic region of the PIN structure. The novel aspect of this detector is that the one surface is divided into a 2D array of pixels, and that the collected holes are divided between a row and a column collector in each pixel, yielding both dimensions of position information from this side of the detector. In a conventional PIN detector, both sides are divided into stripes, and each side provides 1D information. A single large area collector on the opposite side of this new detector is used to determine the energy of the incident nucleus. This scheme requires only a single precision pulse-height amplifier connected to the broad area contract, rather than one for each strip, as in the conventional scheme, resulting in a significant reduction in the mass, power and complexity of the readout electronics. The design, fabrication, and operation of such a detector is discussed. Initial particle tests show a prototype to be functional. The projected power saved by using such as detector is presented.",
"doi": "10.1117/12.187471",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication_date": "1994-09-23"
},
{
"id": "authors:8q8bn-0kc22",
"collection": "authors",
"collection_id": "8q8bn-0kc22",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180724-131524018",
"type": "book_section",
"title": "Cryogenic germanium detectors for a weakly interactive massive particle (WIMP) dark-matter search",
"book_title": "EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy V",
"author": [
{
"family_name": "Stockwell",
"given_name": "W.",
"clpid": "Stockwell-W"
},
{
"family_name": "Akerib",
"given_name": "D.",
"clpid": "Akerib-D-S"
},
{
"family_name": "Aubourg",
"given_name": "\u00c9.",
"clpid": "Aubourg-\u00c9"
},
{
"family_name": "Barnes",
"given_name": "P. D., Jr.",
"clpid": "Barnes-P-D-Jr"
},
{
"family_name": "Cummings",
"given_name": "A.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Da Silva",
"given_name": "A.",
"clpid": "Da-Silva-A"
},
{
"family_name": "Emes",
"given_name": "J.",
"clpid": "Emes-J"
},
{
"family_name": "Golwala",
"given_name": "S.",
"orcid": "0000-0002-1098-7174",
"clpid": "Golwala-S-R"
},
{
"family_name": "Haller",
"given_name": "E. E.",
"clpid": "Haller-E-E"
},
{
"family_name": "Margulies",
"given_name": "S.",
"clpid": "Margulies-S"
},
{
"family_name": "Pritychenko",
"given_name": "B.",
"clpid": "Pritychenko-B"
},
{
"family_name": "Ross",
"given_name": "R. R.",
"clpid": "Ross-R-R"
},
{
"family_name": "Sadoulet",
"given_name": "B.",
"clpid": "Sadoulet-B"
},
{
"family_name": "Shutt",
"given_name": "T.",
"clpid": "Shutt-T"
},
{
"family_name": "Smith",
"given_name": "G.",
"orcid": "0000-0003-4494-8277",
"clpid": "Smith-Graham-P"
},
{
"family_name": "Taylor",
"given_name": "J.",
"clpid": "Taylor-J"
},
{
"family_name": "White",
"given_name": "S.",
"clpid": "White-S"
},
{
"family_name": "Young",
"given_name": "B. A.",
"clpid": "Young-B-A"
}
],
"contributor": [
{
"family_name": "Siegmund",
"given_name": "Oswald H. W.",
"clpid": "Siegmund-O-H-W"
},
{
"family_name": "Vallerga",
"given_name": "John V.",
"clpid": "Vallerga-J-V"
}
],
"abstract": "We are preparing an experimental search for weakly interacting massive particle (WIMP) dark matter using cryogenic germanium detectors. These detectors measure both the ionization and phonons produced by particle interactions in the substrate. The ionization measurement uses low drift fields, approximately equals 1 V/cm. The phonon measurement is made using neutron transmutation doped (NTD) germanium thermistors. Simultaneous detection of phonons and ionization allows us to discriminate between electron-recoil and nuclear-recoil events which gives a powerful method for isolating possible WIMP events (nuclear recoils) from background gamma ray events (electron recoils). Recent work on our understanding and optimization of these detectors will be presented.",
"doi": "10.1117/12.186825",
"isbn": "9780819416049",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_publication": "Bellingham, WA",
"publication_date": "1994-09-16",
"pages": "374-381"
},
{
"id": "authors:9kwrj-27069",
"collection": "authors",
"collection_id": "9kwrj-27069",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140523-101203531",
"type": "article",
"title": "Geomagnetically Trapped Anomalous Cosmic Rays",
"author": [
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "Since its launch in July 1992, the polar-orbiting satellite SAMPEX has been collecting data on geomagnetically trapped heavy ions, predominantly O, N, and Ne, at energies \u2273 15 MeV/nucleon and in a narrow L shell range near L = 2. Their location, elemental composition, energy spectra, pitch angle distribution, and time variations all support the theory that these particles originated as singly ionized interplanetary anomalous cosmic rays that were stripped of electrons in the Earth's upper atmosphere and subsequently trapped. The O are observed primarily at pitch angles outside the atmospheric loss cones, consistent with a trapped population, and their distribution there is nearly isotropic. The abundances relative to O of the N, possibly Ne, and especially C are lower than the corresponding interplanetary values, which may be indicative of the trapping efficiencies. The distributions of trapped N, O, and Ne in energy and L shell suggest that most of the ions observed at the SAMPEX altitude of \u223c600 km are not fully stripped when initially trapped. A comparison of the trapped intensity with the much lower interplanetary intensity of anomalous cosmic rays provides model-dependent estimates of the product of the trapping probability and the average trapped particle lifetime against ionization losses in the residual atmosphere for particles that mirror near the SAMPEX altitude.",
"doi": "10.1029/94JA03140",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "1994-06-01",
"series_number": "A6",
"volume": "100",
"issue": "A6",
"pages": "9503"
},
{
"id": "authors:rvw83-0b451",
"collection": "authors",
"collection_id": "rvw83-0b451",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140520-100248179",
"type": "article",
"title": "Distance to the Solar Wind Termination Shock and the Source Flux of Anomalous Cosmic Rays During 1986-1988",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "We use observations of the intensity of anomalous cosmic ray helium and oxygen in the outer heliosphere near the last solar minimum period, in conjunction with solar observations of the tilt of the neutral current sheet, to estimate that the solar wind termination shock was at 67 \u00b1 5 AU during the time period 1986.7-1988.5. We find the source flux of anomalous cosmic rays at the shock to be 1.7 \u00b1 0.3 (m\u00b2 s sr MeV/nucleon)^(\u22121) for 7.1-17.1 MeV/nucleon anomalous cosmic ray oxygen and 4.3 \u00b1 0.8 (m\u00b2 s sr MeV/nucleon)^(\u22121) for 31-57 MeV/nucleon anomalous cosmic ray helium. We also estimate a source flux of anomalous cosmic ray hydrogen of 2.3 \u00b1 0.6 (m\u00b2 s sr MeV)^(\u22121) at 134 MeV. The resulting energy density of anomalous cosmic rays at the solar wind termination shock is \u223c0.03 eV/cm\u00b3, approximately 2% of the energy density of the solar wind at 67 AU.",
"doi": "10.1029/94JA00551",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "1994-06",
"series_number": "A6",
"volume": "99",
"issue": "A6",
"pages": "11547-11552"
},
{
"id": "authors:qt61x-72b60",
"collection": "authors",
"collection_id": "qt61x-72b60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140516-132152344",
"type": "article",
"title": "Anomalous Cosmic Rays: Interstellar Interlopers in the Heliosphere and Magnetosphere",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "Since the beginning of the space age, it\nwas known that two main sources of energetic\nparticles pervade interplanetary space:\ngalactic cosmic rays (GCRs), which originate\nin sources outside the solar system, and solar energetic particles (SEPs), associated\nwith transient events on the Sun.\nBut over 20 years ago, instruments on the\nPioneer 1O, IMP 5, and IMP 7 spacecraft discovered\na third component of energetic particles\nknown as \"anomalous cosmic rays,\"\nthat represents a sample of nearby interstellar\nmaterial.\nOver the past 2 decades, ACRs have been\nused to study the acceleration and transport\nof energetic particles within the solar system,\ndeduce the global properties of the heliosphere-\nthe bubble of solar wind that envelopes\nthe solar system, and study the\ninterstellar material itself.\nIt has recently been shown that some of\nthese ACRs have become trapped in Earth's\nmagnetic field, where they form a radiation\nbelt composed of interstellar material (Figure\nI). Also, ACRs are being used to address a\nquestion that has existed ever since the discovery\nof the solar wind: \"How large is the\nheliosphere?\"",
"doi": "10.1029/94EO00864",
"issn": "0096-3941",
"publisher": "American Geophysical Union",
"publication": "Eos",
"publication_date": "1994-04-19",
"series_number": "16",
"volume": "75",
"issue": "16",
"pages": "185-193"
},
{
"id": "authors:960yq-3t819",
"collection": "authors",
"collection_id": "960yq-3t819",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140512-104159363",
"type": "article",
"title": "Development of an Interdigitated Pixel PIN Detector for Energetic Particle Spectroscopy in Space",
"author": [
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Rosenberg",
"given_name": "J. J.",
"clpid": "Rosenberg-J-J"
},
{
"family_name": "Cunningham",
"given_name": "T. J.",
"clpid": "Cunningham-T-J"
},
{
"family_name": "Mazed",
"given_name": "M.",
"clpid": "Mazed-M"
},
{
"family_name": "Holtzman",
"given_name": "M. J.",
"clpid": "Holtzman-M-J"
},
{
"family_name": "Fossum",
"given_name": "E. R.",
"clpid": "Fossum-E-R"
}
],
"abstract": "The development of a new two\u2010dimensional position\u2010sensitive detector for use in space\u2010borne energetic particle spectrometers is described. The novel feature of this device is the use of interdigitated pixels to provide both dimensions of position information from a single side of the detector, while a measurement of the energy deposition is derived from the opposite side. The advantage of this approach is that both good position resolution and excellent energy resolution can be achieved while at the same time realizing significant reductions in the complexity, power, and weight of the associated read\u2010out electronics.",
"doi": "10.1080/02757259309532200",
"issn": "0275-7257",
"publisher": "Taylor & Francis",
"publication": "Remote Sensing Reviews",
"publication_date": "1994",
"series_number": "1-3",
"volume": "8",
"issue": "1-3",
"pages": "245-253"
},
{
"id": "authors:0pekb-t8g18",
"collection": "authors",
"collection_id": "0pekb-t8g18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140612-111816582",
"type": "article",
"title": "SAMPEX Measurements of Heavy Ions Trapped in the Magnetosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Blake",
"given_name": "J. B.",
"clpid": "Blake-J-B"
}
],
"abstract": "New observations of >15 MeV/nuc trapped heavy ions\nwith Z 2 2 have been made by the SAMPEX spacecraft in low\npolar orbit. The composition of these ions, which are located\nprimarily around L = 2, is dominated by He, N, O, and Ne.\nThe N, O, and Ne ions are apparently trapped \"anomalous\ncosmic rays,\" while the origin of the trapped He flux is\npresently uncertain. These ions can affect the rate of single-event\nupsets (SEUs) in spacecraft hardware.",
"doi": "10.1109/23.273518",
"issn": "0018-9499",
"publisher": "IEEE",
"publication": "IEEE Transactions on Nuclear Science",
"publication_date": "1993-12",
"series_number": "6",
"volume": "40",
"issue": "6",
"pages": "1458-1462"
},
{
"id": "authors:xs10g-8mx27",
"collection": "authors",
"collection_id": "xs10g-8mx27",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140516-110810887",
"type": "article",
"title": "Coronal Abundances of Neon and Magnesium Isotopes from Solar Energetic Particles",
"author": [
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The relative abundances of 22 to 70 Me V nucleon^(-l) Ne and Mg isotopes from two large flare-associated\nsolar energetic particle (SEP) events in 1992 October and November, are determined from data taken by the\nMass Spectrometer Telescope on the polar-orbiting SAMPEX satellite. After converting the measured abundances\nto coronal values, the average ^(22)Ne/^(20)Ne ratio is 0.076 \u00b1 0.008, consistent with the solar wind value of\n0.073 but significantly less than that of previous SEP measurements, in which the abundance of ^(22)Ne was\nsubstantially enhanced. The average ^(26)Mg/^(24)Mg ratio is 0.152 \u00b1 0.012, consistent with both previous SEP and\nother solar system measurements.",
"doi": "10.1086/187112",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "1993-11-20",
"series_number": "1",
"volume": "418",
"issue": "1",
"pages": "L45-L48"
},
{
"id": "authors:3bfrs-97g72",
"collection": "authors",
"collection_id": "3bfrs-97g72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140520-091404026",
"type": "article",
"title": "The Return of the Anomalous Cosmic Rays to 1 AU in 1992",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Klecker",
"given_name": "B.",
"clpid": "Klecker-B"
},
{
"family_name": "Hovestadt",
"given_name": "D.",
"clpid": "Hovestadt-D"
},
{
"family_name": "Scholer",
"given_name": "M.",
"clpid": "Scholer-M"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "Mazur",
"given_name": "J. E.",
"clpid": "Mazur-J-E"
},
{
"family_name": "Hamilton",
"given_name": "D. C.",
"clpid": "Hamilton-D-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Blake",
"given_name": "J. B.",
"clpid": "Blake-J-B"
}
],
"abstract": "New observations of low energy (approximately 1 to 200 MeV/nuc) cosmic rays measured by three newly launched experiments on Solar, Anomalous, and Magnetospheric Particle Explorer (SAMPEX) during 1992 and 1993 show the strong presence of anomalous cosmic ray (ACR) nitrogen and oxygen, well before the approaching solar minimum. When compared with ACR temporal variations over the past two solar cycles we find that the 1992-1993 fluxes are approximately 5 to 10 times their level at corresponding neutron monitor counting rates in 1969-1970 and 1985",
"doi": "10.1029/93GL02493",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1993-10-22",
"series_number": "20",
"volume": "20",
"issue": "20",
"pages": "2263-2266"
},
{
"id": "authors:dz0nv-fm396",
"collection": "authors",
"collection_id": "dz0nv-fm396",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161018-131737795",
"type": "book_section",
"title": "Cosmic-ray detector with interdigitated-finger pixels for two-dimensional position information from a single wafer side",
"book_title": "Astroparticle Physics and Novel Gamma-Ray Telescopes",
"author": [
{
"family_name": "Cunningham",
"given_name": "Thomas J.",
"clpid": "Cunningham-T-J"
},
{
"family_name": "Mazed",
"given_name": "Mohaminad",
"clpid": "Mazed-M"
},
{
"family_name": "Holtzman",
"given_name": "Melinda J.",
"clpid": "Holtzman-M-J"
},
{
"family_name": "Fossum",
"given_name": "Eric R.",
"clpid": "Fossum-E-R"
},
{
"family_name": "Cook",
"given_name": "Walter R., III",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "Alan C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "Richard A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
}
],
"contributor": [
{
"family_name": "Cline",
"given_name": "David B.",
"clpid": "Cline-D-B"
}
],
"abstract": "This paper describes a type of cosmic ray detector for isotopic and energy detection of energetic nuclei which derives both dimensions of position information from one side of the detector. This simplifies the required readout electronics, since only one precision amplifier connected to the other side is required for an accurate detection of the energy loss. Two dimensional readout is enabled by the use of pixels consisting of closely spaced interdigitated electrodes alternately connected to row and column lines. Spreading of the charge produced by the cosmic ray results in the charge being collected by more than one electrode producing both a row and column signal on one side of the detector. The design, fabrication, and characterization of the interdigitated-pixel detector is discussed.",
"doi": "10.1117/12.161384",
"isbn": "9780819411846",
"publisher": "Society of Photo-optical Instrumentation Engineers",
"place_of_publication": "Bellingham, WA",
"publication_date": "1993-10-19",
"pages": "15-22"
},
{
"id": "authors:sn8vv-a9r24",
"collection": "authors",
"collection_id": "sn8vv-a9r24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140520-095742074",
"type": "article",
"title": "SAMPEX Observations of Anomalous Cosmic Rays Trapped in the Magnetosphere",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"abstract": "The Solar, Anomalous, and Magnetospheric Particle Explorer (SAMPEX),\nlaunched July 3, 1992, into an 82 degree inclination, low-Earth orbit (670 x\n520 km), is the first of NASA's new line of Small Explorer (SMEX) missions.\nSAMPEX has been described in U.S. STEP News, Vol. 1, No. 6, December\n1991. The spacecraft carries four instruments designed to measure\nthe composition of energetic nuclei and electrons over a broad range in energy\nand intensity, including particles of solar, interplanetary, galactic,\nand magnetospheric origin. A detailed description of the spacecraft and\nthese instruments is given in the May 1993 issue of Geoscience and Remote\nSensing. Of the many studies that SAMPEX has conducted during its first\nyear of operation, one of the most interesting has been of a trapped radiation\nbelt encircling the Earth that contains high-energy N, 0, and Ne nuclei\nfrom the local interstellar medium. These observations, along with\nearlier work from a series of COSMOS satellites, confirm a prediction\nmade more than a decade ago. The process by which interste1lar material\nfinds its way into the magnetosphere involves a rather fascinating series of\nsteps.",
"publisher": "STEP International",
"publication": "STEP International",
"publication_date": "1993-10",
"series_number": "10",
"volume": "3",
"issue": "10",
"pages": "1-4"
},
{
"id": "authors:v8nss-m3g72",
"collection": "authors",
"collection_id": "v8nss-m3g72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140304-145352097",
"type": "article",
"title": "New evidence for geomagnetically trapped anomalous cosmic rays",
"author": [
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "We report new observations of \u2265 15 MeV/nuc trapped heavy ions with Z \u2265 2, made on the polar-orbiting SAMPEX spacecraft in late 1992 and early 1993. A trapped population that includes He, N, O, and Ne is found to be located at L \u2248 2. We conclude that the observed N, O, and Ne ions are \"anomalous\" cosmic rays, trapped by the mechanism proposed by Blake and Friesen. While it is not expected that this mechanism would also trap anomalous He, the characteristics of the trapped He population are generally consistent with those of N, O, and Ne.",
"doi": "10.1029/93GL01961",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1993-09-15",
"series_number": "18",
"volume": "20",
"issue": "18",
"pages": "2003-2006"
},
{
"id": "authors:fbwg7-htz45",
"collection": "authors",
"collection_id": "fbwg7-htz45",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140516-103709418",
"type": "article",
"title": "Estimate of the Distance to the Solar Wind Termination Shock from Gradients of Anomalous Cosmic Ray Oxygen",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "The radial gradient of anomalous cosmic ray oxygen measured instantaneously between Voyager 2 and Pioneer 10 during 1985-1988 is correlated with the inferred tilt of the heliospheric neutral sheet. This is consistent with a simple model in which the radial gradient is related to the length of the neutral sheet between the two spacecraft. With this model we show that the radial gradient and the tilt of the neutral sheet near the solar wind termination shock can be inferred from the Voyager and Pioneer observations. By comparing the time history of the inferred tilt with that derived from solar observations, we estimate that the termination shock was at 62 +5/-7 AU at solar minimum in 1987. At solar maximum the shock should be located at about 90 AU due to the increased pressure of the solar wind.",
"doi": "10.1029/93JA01173",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research B",
"publication_date": "1993-09-01",
"series_number": "A9",
"volume": "98",
"issue": "A9",
"pages": "15,165-15,168"
},
{
"id": "authors:ksf0f-fqx51",
"collection": "authors",
"collection_id": "ksf0f-fqx51",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-081705878",
"type": "book_section",
"title": "New Evidence for Anomalous Cosmic Rays Trapped in the Magnetosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Leahy",
"given_name": "D. A.",
"clpid": "Leahy-D-A"
},
{
"family_name": "Hickws",
"given_name": "R. B.",
"clpid": "Hickws-R-B"
},
{
"family_name": "Venkatesan",
"given_name": "D.",
"clpid": "Venkatesan-D"
}
],
"abstract": "We report new observations of \u2265 15 MeV/nuc trapped heavy ions with Z \u2265 2, made on\nthe polar-orbiting SAMPEX spacecraft in late 1992. A trapped population, located\nprimarily near the SAA, includes He, N, O, and Ne. We conclude that they are\n\"anomalous\" cosmic rays trapped by the mechanism proposed by Blake and Friesen.",
"publisher": "University of Calgary",
"publication_date": "1993-07"
},
{
"id": "authors:6tqe9-1n669",
"collection": "authors",
"collection_id": "6tqe9-1n669",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-092741225",
"type": "book_section",
"title": "Isotopic Composition of Solar Energetic Particles Observed in the October/November, 1992 Solar Flares",
"author": [
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Leahy",
"given_name": "D. A.",
"clpid": "Leahy-D-A"
},
{
"family_name": "Hickws",
"given_name": "R. B.",
"clpid": "Hickws-R-B"
},
{
"family_name": "Venkatesan",
"given_name": "D.",
"clpid": "Venkatesan-D"
}
],
"abstract": "We report on abundances of >20 MeV/nuc Ne and Mg isotopes measured during\ntwo large solar flares in October and November, 1992, by the Mass Spectrometer\nTelescope on SAMPEX. The observed ^(22)Ne/^(20)Ne ratio of -0.07 is consistent with\nthe solar wind value of 0.073, in contrast to previous SEP measurements in which\n^(22)Ne was substantially enhanced.",
"publisher": "University of Calgary",
"publication_date": "1993-07"
},
{
"id": "authors:1qjyc-4mm98",
"collection": "authors",
"collection_id": "1qjyc-4mm98",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-082424248",
"type": "book_section",
"title": "The Distance to the Solar Wind Termination Shock During 1986 - 1988",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Leahy",
"given_name": "D. A.",
"clpid": "Leahy-D-A"
},
{
"family_name": "Hickws",
"given_name": "R. B.",
"clpid": "Hickws-R-B"
},
{
"family_name": "Venkatesan",
"given_name": "D.",
"clpid": "Venkatesan-D"
}
],
"abstract": "We use observations of the intensity of anomalous cosmic ray oxygen in the outer\nheliosphere near the last solar minimum period, in conjunction with observations\nof the average tilt of the neutral current sheet, to estimate that the solar wind termination\nshock was at 62 \u00b1 2 AU during the time period 1986.5 - 1988.5 and that\nthe flux of 7.1 - 17.1 MeV/nuc anomalous cosmic ray oxygen at the shock was\n1.27 \u00b1 0.04 p/m^2 sec sr MeV/nuc.",
"publisher": "University of Calgary",
"publication_date": "1993-07"
},
{
"id": "authors:p1kej-7c243",
"collection": "authors",
"collection_id": "p1kej-7c243",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-082936422",
"type": "book_section",
"title": "The Return of the Anomalous Component to 1 AU in 1992",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Leahy",
"given_name": "D. A.",
"clpid": "Leahy-D-A"
},
{
"family_name": "Hickws",
"given_name": "R. B.",
"clpid": "Hickws-R-B"
},
{
"family_name": "Venkatesan",
"given_name": "D.",
"clpid": "Venkatesan-D"
}
],
"abstract": "New observations of low energy (15 to 200 MeV/nuc) cosmic rays from SAMPEX\nshow the strong presence of anomalous cosmic ray (ACR) N, O, and Ne, well before\nthe approaching solar minimum. When compared with ACR temporal variations over\nthe past two solar cycles we find that the 1992 fluxes are ~5 to 10 times their level at\ncorresponding neutron monitor counting rates in 1969-1970 and 1985.",
"publisher": "University of Calgary",
"publication_date": "1993-07"
},
{
"id": "authors:qy6rr-f2239",
"collection": "authors",
"collection_id": "qy6rr-f2239",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-113840884",
"type": "book_section",
"title": "Measurements of the Composition of Galactic Cosmic Rays on SAMPEX",
"author": [
{
"family_name": "Leske",
"given_name": "R. A.",
"orcid": "0000-0002-0156-2414",
"clpid": "Leske-R-A"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Leahy",
"given_name": "D. A.",
"clpid": "Leahy-D-A"
},
{
"family_name": "Hickws",
"given_name": "R. B.",
"clpid": "Hickws-R-B"
},
{
"family_name": "Venkatesan",
"given_name": "D.",
"clpid": "Venkatesan-D"
}
],
"abstract": "The Mass Spectrometer Telescope (MAST) on board the Solar, Anomalous, and\nMagnetospheric Particle Explorer (SAMPEX) satellite is designed to make high\nresolution measurements of the elemental and isotopic composition of cosmic rays\nfrom ~C to Ni over the energy interval of ~15 to 300 MeV per nucleon. At this\nconference, we will present a preliminary look at the composition of galactic cosmic\nrays as measured with this instrument, based on approximately the first 6 months of\ndata.",
"publisher": "University of Calgary",
"publication_date": "1993-07"
},
{
"id": "authors:3e6s9-27q49",
"collection": "authors",
"collection_id": "3e6s9-27q49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140512-103823930",
"type": "article",
"title": "PET: A Proton/Electron Telescope for Studies of Magnetospheric, Solar, and Galactic Particles",
"author": [
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Baker",
"given_name": "D. N.",
"clpid": "Baker-D-N"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Blake",
"given_name": "J. B.",
"clpid": "Blake-J-B"
},
{
"family_name": "Callis",
"given_name": "L. B.",
"clpid": "Callis-L-B"
}
],
"abstract": "The proton/electron telescope (PET) on SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) is designed to provide measurements of energetic electrons and light nuclei from solar, Galactic, and magnetospheric sources. PET is an all solid-state system that will measure the differential energy spectra of electrons from ~1 to ~30 MeV and H and He nuclei from ~20 to ~300 MeV/nucleon, with isotope resolution of H and He extending from ~20 to ~80 MeV/nucleon. As SAMPEX scans all local times and geomagnetic cutoffs over the course of its near-polar orbit, PET will characterize precipitating relativistic electron events during periods of declining solar activity, and it will examine whether the production rate of odd nitrogen and hydrogen molecules in the middle atmosphere by precipitating electrons is sufficient to affect O_3 depletion. In addition, PET will complement studies of the elemental and isotopic composition of energetic heavy (Z>2) nuclei on SAMPEX by providing measurements of H, He, and electrons. Finally, PET has limited capability to identify energetic positrons from potential natural and man-made sources.",
"doi": "10.1109/36.225523",
"issn": "0196-2892",
"publisher": "IEEE Transactions on Geoscience and Remote Sensing",
"publication": "IEEE Transactions on Geoscience and Remote Sensing",
"publication_date": "1993-05",
"series_number": "3",
"volume": "31",
"issue": "3",
"pages": "565-571"
},
{
"id": "authors:5ybza-tm133",
"collection": "authors",
"collection_id": "5ybza-tm133",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140307-151617567",
"type": "article",
"title": "MAST: a mass spectrometer telescope for studies of the isotopic composition of solar, anomalous, and galactic cosmic ray nuclei",
"author": [
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"abstract": "The mass spectrometer telescope (MAST) on SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) is designed to provide high-resolution measurements of the isotopic composition of energetic nuclei from He to Ni (Z=2 to 28) over the energy range from ~10 to several hundred MeV/nucleon. During large solar flares MAST will measure the isotopic abundances of solar energetic particles to determine directly the composition of the solar corona, while during solar quiet times MAST will study the isotopic composition of galactic cosmic rays. In addition, MAST will measure the isotopic composition of both interplanetary and trapped fluxes of anomalous cosmic rays, believed to be a sample of the nearby interstellar medium.",
"doi": "10.1109/36.225522",
"issn": "0196-2892",
"publisher": "IEEE",
"publication": "IEEE Transactions on Geoscience and Remote Sensing",
"publication_date": "1993-05",
"series_number": "3",
"volume": "31",
"issue": "3",
"pages": "557-564"
},
{
"id": "authors:xzdn7-a5e93",
"collection": "authors",
"collection_id": "xzdn7-a5e93",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140516-113451049",
"type": "book_section",
"title": "Custom Analog VLSI for the Advanced Composition Explorer (ACE)",
"author": [
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Kecman",
"given_name": "B.",
"clpid": "Kecman-B"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Aalami",
"given_name": "D.",
"clpid": "Aalami-Dean"
},
{
"family_name": "Kleinfelder",
"given_name": "S.A.",
"clpid": "Kleinfelder-S-A"
},
{
"family_name": "Marshall",
"given_name": "J.H.",
"clpid": "Marshall-J-H"
}
],
"editor": [
{
"family_name": "Tsurutani",
"given_name": "B. T.",
"clpid": "Tsurutani-B-T"
}
],
"abstract": "Two custom analog VLSI chips are currently in development for scientific payloads\nof NASA's Advanced Composition Explorer. One chip will be fabricated in the radiation\nhard 1.2 um CMOS process of the United Technologies Microelectronics Center (UlMC),\nand will contain 16 complete discriminator/12 bit pulse-height-analysis chains for the\nreadout of heavy ion Si strip detectors. The second chip will be fabricated by Harris\nSemiconductor in their dielectrically isolated bipolar VHF process. This chip will contain\nthe active elements of a single precision pulse-height-analysis chain and several precision\ndiscriminator chains. The chips designed in this effort and the techniques employed are\nexpected to be applicable in science payloads of future missions, especially those which\nplace extraordinary premiums on weight, power, and/or performance.",
"publisher": "Jet Propulsion Laboratory",
"publication_date": "1993"
},
{
"id": "authors:4zgjm-f1143",
"collection": "authors",
"collection_id": "4zgjm-f1143",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141021-155634792",
"type": "book_section",
"title": "Detection Efficiency of the CRIS Scintillating Optical Fiber Hodoscope",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Crary",
"given_name": "D. J.",
"clpid": "Crary-D-J"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Geer",
"given_name": "L. Y.",
"clpid": "Geer-L-Y"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Lawrence",
"given_name": "David J.",
"clpid": "Lawrence-D-J"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
}
],
"contributor": [
{
"family_name": "Leahy",
"given_name": "D. A.",
"clpid": "Leahy-D-A"
},
{
"family_name": "Hickws",
"given_name": "R. B.",
"clpid": "Hickws-R-B"
},
{
"family_name": "Venkatesan",
"given_name": "D.",
"clpid": "Venkatesan-D"
}
],
"abstract": "Measurements of the detection efficiency of a Scintillating Optical Fiber Trajectory (SOFT) detector for 660 MeV/n Carbon, Boron, Beryllium and Lithium nuclei and for 300 MeV/n Fe nuclei are described. Detection efficiencies of 99.8%, 98.7%, 97.5%, and 93.8% for C, B, Be, and Li respectively were obtained for a single layer of fibers at an angle of incidence of 30\u00b0. These fibers had a black coating of extramural absorber (EMA) to optically decouple the fibers. Somewhat better detection efficiencies were obtained for optically coupled fibers (no EMA). The\ndetection efficiencies for iron nuclei were ~99.7%. We have used these results to estimate the event detection efficiencies of the fiber hodoscope which is planned for\nuse in the Cosmic Ray Isotope Spectrometer (CRIS) (Stone, et al., 1989) experiment on the Advanced Composition Explorer (ACE). We find that for the highest energy\nLithium nuclei which will stop in CRIS, the detection efficiency is about 89% for 6 plane events and about 99% for 5 plane events at 30\u00b0.",
"publisher": "World Scientific",
"publication_date": "1993"
},
{
"id": "authors:961jz-90r15",
"collection": "authors",
"collection_id": "961jz-90r15",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141022-095413422",
"type": "book_section",
"title": "SAMPEX Observations of Geomagnetically Trapped Anomalous Cosmic Rays",
"author": [
{
"family_name": "Cummings",
"given_name": "J. R.",
"clpid": "Cummings-J-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
}
],
"contributor": [
{
"family_name": "Leahy",
"given_name": "D. A.",
"clpid": "Leahy-D-A"
},
{
"family_name": "Hickws",
"given_name": "R. B.",
"clpid": "Hickws-R-B"
},
{
"family_name": "Venkatesan",
"given_name": "D.",
"clpid": "Venkatesan-D"
}
],
"abstract": "We summarize observations of trapped anomalous cosmic rays made with the Mass Spectrometer Telescope (MASn on the polar-orbiting SAMPEX spacecraft during late 1992 and early 1993. MAST observes a trapped population of heavy ions with ~15 MeV/nuc that includes N, 0, and Ne, but very little C, located in a narrow belt at L=2. The characteristics of\nthis radiation belt are generally consistent with those expected from the mechanism proposed by Blake and Friesen for trapping anomalous cosmic rays in the magnetosphere and with COSMOS observations made during the last solar minimum. We discuss the location, composition, and temporal history of the trapped heavy ions observed with SAMPEX and\ncompare them with properties of anomalous cosmic rays observed in the interplanetary medium. Although trapped He ions are also observed by MAST, it appears likely that they\nhave a different origin.",
"publisher": "World Scientific",
"publication_date": "1993"
},
{
"id": "authors:z8wav-rj233",
"collection": "authors",
"collection_id": "z8wav-rj233",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140516-114149179",
"type": "book_section",
"title": "An Interdigitated Pixel PIN Detector for Energetic Particle Spectroscopy in Space",
"author": [
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Cunningham",
"given_name": "T. J.",
"clpid": "Cunningham-T-J"
},
{
"family_name": "Mazed",
"given_name": "M.",
"clpid": "Mazed-M"
},
{
"family_name": "Fossum",
"given_name": "E. R.",
"clpid": "Fossum-E-R"
}
],
"contributor": [
{
"family_name": "Tsurutani",
"given_name": "B. T.",
"clpid": "Tsurutani-B-T"
}
],
"abstract": "We describe a new two-dimensional position-sensitive detector, now under\ndevelopment, for use in space-borne energetic particle spectrometers. The novel\nfeature of this device is the use of interdigitated pixels to provide both dimensions of\nposition information from a single side of the detector, while a measurement of the\nenergy deposition is derived from the opposite side. An advantage of this approach is\nthat significant reductions in the complexity, power, and weight of the associated\nread-out electronics can be realized without sacrificing position or energy resolution.",
"publisher": "National Aeronautics Space Division",
"publication_date": "1993"
},
{
"id": "authors:3phjr-a2w10",
"collection": "authors",
"collection_id": "3phjr-a2w10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140512-100311515",
"type": "article",
"title": "A Bevalac Calibration of a Scintillating Optical Fiber Hodoscope",
"author": [
{
"family_name": "Crary",
"given_name": "D. J.",
"clpid": "Crary-D-J"
},
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Lawrence",
"given_name": "D. J.",
"clpid": "Lawrence-D-J"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
}
],
"abstract": "As part of instrument definition activities for the Advanced Composition Explorer (ACE) we have evaluated a hodoscope comprised of scintillating fibers for possible use in the Cosmic Ray Isotope Spectrometer (CRIS). The hodoscope would determine the trajectories of individual cosmic ray nuclei with 3 \u2a7d Z \u2a7d 40 and energies up to several hundred MeV/n which stop in four silicon solid state telescopes. We report on the analysis of data from a December 1990 Bevalac calibration of a CRIS test model in which the hodoscope consisted of 200 \u03bcm, square cross section, scintillating fibers, and which used silicon detectors for dE/dx - E_(Tot) measurements. The positional resolution obtained with the fiber hodoscope was \u223c 60 \u03bcmfor iron nuclei at angles from 0\u201330\u00b0 with respect to the normal to the fiber planes. The detection efficiency for iron and silicon nuclei was determined to be > 99% for beam angles of \u2a7e 20\u00b0.",
"doi": "10.1016/0168-9002(92)90915-Q",
"issn": "0168-9002",
"publisher": "Elsevier",
"publication": "Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment",
"publication_date": "1992-06-01",
"series_number": "2-3",
"volume": "A316",
"issue": "2-3",
"pages": "311-317"
},
{
"id": "authors:00zk9-74d35",
"collection": "authors",
"collection_id": "00zk9-74d35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140805-202852761",
"type": "book_section",
"title": "The Physical Significance of 'Shifted' Gradients and the Location of the Solar Wind Termination Shock",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "We use observations of anomalous cosmic-ray (ACR) oxygen from the cosmic-ray experiments on the Voyager 2 (V2) and Pioneer IO (PIO) spacecraft during 1985-1988 to\ninvestigate the physical significance of the \"shifted\" radial gradient The \"shifted\" gradient is computed by comparing fluxes measured at different times at the two spacecraft to \"correct\" for the propagation delay of solar modulation. We use a simple model of particle propagation in which the flow is inwards along the wavy neutral sheet to suggest that for qA < 0 near solar minimum conditions the \"shifted\" gradient is a measure of the gradient\nnear the solar wind termination shock. This simple model leads to an estimate of the location of the termination shock at 55 (+9/-5) AU, suggesting that the shock could be encountered within this decade.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1991"
},
{
"id": "authors:ap4t5-agk04",
"collection": "authors",
"collection_id": "ap4t5-agk04",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141007-134109460",
"type": "book_section",
"title": "A Bevalac Calibration of a Scintillating Optical Fiber Hodoscope for Possible use on the Advanced Composition Explorer",
"author": [
{
"family_name": "Binns",
"given_name": "W. R.",
"orcid": "0000-0001-6110-3407",
"clpid": "Binns-W-R"
},
{
"family_name": "Crary",
"given_name": "D. J.",
"clpid": "Crary-D-J"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Klarmann",
"given_name": "J.",
"clpid": "Klarmann-J"
},
{
"family_name": "Lawrence",
"given_name": "D. J.",
"clpid": "Lawrence-D-J"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
}
],
"abstract": "As part of instrument definition activities for the Advanced\nComposition Explorer (ACE) we are evaluating a hodoscope comprised of scintillating fibers for possible use in the Cosmic Ray Isotope Spectrometer (CRIS). The hodoscope would determine the trajectories of individual cosmic ray nuclei which stop in the silicon solid state telescopes in CRIS. We\nreport a preliminary analysis of data from a Dec., 1990 Bevalac calibration of a CRIS test model which consisted of a scintillating fiber hodosccpe, utilizing 200mm, square cross section scintillating fibers, and silicon detectors for dE/dx-Erot measurements. The positional resolution obtained in our preliminary data analysis is -60\u03bcm for angles from 0-30\u00b0. The detection efficiency for iron and silicon nuclei was determined to be >99% for beam angles of \u2265 20\u00b0.",
"publisher": "International Union of Pure and Applied Physics",
"publication_date": "1991"
},
{
"id": "authors:4vb45-3yb48",
"collection": "authors",
"collection_id": "4vb45-3yb48",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140924-095030514",
"type": "book_section",
"title": "The Isotopic Composition of Anomalous Cosmic Ray Neon",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "We have used observations of neon in the energy interval 14.6 - 35.6 MeV /nuc from the cosmic-ray experiment on the Voyager 2 (V2) spacecraft during 1986-1988 to\nderive the ^(22)Ne/^(20)Ne ratio for the source material of the anomalous cosmic rays (ACRs). Because of the relatively small contamination from galactic cosmic-ray (CCR) neon during the time period selected, we have significantly improved the precision with which this ratio is known. We find that the derived ACR source ratio, ^(22)Ne/^(20)Ne = 0.077 +0.068/-0.043, is consistent with the composition of the solar wind (0.073) and meteoritic neon-A (0.12), but inconsistent with the galactic cosmic ray source (0.43). This finding places new limits on the possible source material of the anomalous component. If the anomalous component does derive from the inward flowing interstellar neutral gas, then the composition of the source of galactic cosmic rays differs from that of the very local interstellar medium (VLISM).",
"publisher": "Institute for Advanced Studies",
"publication_date": "1991"
},
{
"id": "authors:2t45p-h2q62",
"collection": "authors",
"collection_id": "2t45p-h2q62",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140924-091647751",
"type": "book_section",
"title": "The Physical Significance of 'Shifted' Gradients and the Location of the Solar Wind Termination Shock",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "We use observations of anomalous cosmic-ray (ACR) oxygen from the cosmic-ray experiments on the Voyager 2 (V2) and Pioneer IO (PIO) spacecraft during 1985-1988 to investigate the physical significance of the \"shifted\" radial gradient The \"shifted\" gradient is computed by comparing fluxes measured at different times at the two spacecraft to \"correct\" for the propagation delay of solar modulation. We use a simple model of particle propagation in which the flow is inwards along the wavy neutral sheet to suggest that for qA < 0 near solar minimum conditions the \"shifted\" gradient is a measure of the gradient\nnear the solar wind termination shock. This simple model leads to an estimate of the location of the termination shock at 55(+9/-5) AU, suggesting that the shock could be encountered within this decade.",
"publisher": "Institute for Advanced Studies",
"publication_date": "1991"
},
{
"id": "authors:2r6xp-myb97",
"collection": "authors",
"collection_id": "2r6xp-myb97",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140715-154126254",
"type": "book_section",
"title": "The Advanced Composition Explorer",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Feldman",
"given_name": "W. C.",
"clpid": "Feldman-W-C"
},
{
"family_name": "Frain",
"given_name": "W. E.",
"clpid": "Frain-W-E"
},
{
"family_name": "Geissman",
"given_name": "J.",
"clpid": "Geissman-J-W"
},
{
"family_name": "Gloeckler",
"given_name": "G.",
"clpid": "Gloeckler-G"
},
{
"family_name": "Gold",
"given_name": "R. E.",
"clpid": "Gold-R-E"
},
{
"family_name": "Hovestadt",
"given_name": "D.",
"clpid": "Hovestadt-D"
},
{
"family_name": "Krimigis",
"given_name": "S. M.",
"orcid": "0000-0003-2781-2386",
"clpid": "Krimigis-S-M"
},
{
"family_name": "Mason",
"given_name": "G. M.",
"orcid": "0000-0003-2169-9618",
"clpid": "Mason-G-M"
},
{
"family_name": "McComas",
"given_name": "D.",
"orcid": "0000-0001-6160-1158",
"clpid": "McComas-D-J"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Simpson",
"given_name": "J. A.",
"clpid": "Simpson-J-A"
},
{
"family_name": "von Rosenvinge",
"given_name": "T. T.",
"clpid": "von-Rosenvinge-T-T"
},
{
"family_name": "Wiedenbeck",
"given_name": "M. E.",
"orcid": "0000-0002-2825-3128",
"clpid": "Wiedenbeck-M-E"
}
],
"contributor": [
{
"family_name": "Jones",
"given_name": "W. V.",
"clpid": "Jones-W-V"
},
{
"family_name": "Kerr",
"given_name": "Frank J.",
"clpid": "Kerr-F-J"
},
{
"family_name": "Ormes",
"given_name": "J. F.",
"clpid": "Ormes-J-F"
}
],
"abstract": "The Advanced Composition Explorer (ACE) was recently selected as one of two new Explorer\u2010class missions to be developed for launch during the mid\u20101990's ACE will observe particles of solar, interplanetary, interstellar, and galactic origins, spanning the energy range from that of the solar wind (\u223c1 keV/nucleon) to galactic cosmic ray energies (several hundred MeV/nucleon). Definitive studies will be made of the abundance of nearly all isotopes from H to Zn (1\u2264Z\u226430), with exploratory isotope studies extending to Zr(Z=40). To accomplish this, the ACE payload includes six high\u2010resolution spectrometers, each designed to provide the optimum charge, mass, or charge\u2010state resolution in its particular energy range, and each having a geometry factor optimized for the expected flux levels, so as to provide a collecting power a factor of 10 to 1000 times greater than previous or planned experiments. The payload also includes several instruments of standard design that will monitor solar wind and magnetic field conditions and energetic H, He, and electron fluxes. We summarize here the scientific objectives, instrumentation, spacecraft, and mission approach that were defined for ACE during the Phase\u2010A study period.",
"doi": "10.1063/1.39173",
"publisher": "American Institute of Physics",
"publication_date": "1990-03-20"
},
{
"id": "authors:4n49x-9pd44",
"collection": "authors",
"collection_id": "4n49x-9pd44",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140714-155936587",
"type": "book_section",
"title": "Radial and Latitudinal Gradients of Anomalous Cosmic-Ray Oxygen and Helium from 1 to ~41 AU",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Protheroe",
"given_name": "Raymond J.",
"clpid": "Protheroe-R-J"
}
],
"abstract": "We have used data from the IMP 8, Voyager 1 (VI), Voyager 2 (V2), Pioneer 11 (Pll), and Pioneer 10 (PIO) spacecraft. to determine the radial and latitudinal gradients of\nanomalous cosmic ray oxygen in the energy range ~7 - 25 MeV/nuc and anomalous cosmic\nray helium in the energy range ~20- 25 MeV/nuc for a time period near minimum solar\nmodulation in 1987. We find that the radial gradients of both species are decreasing functions\nof radial distance, r, approximately r^(-1) for oxygen and r^(-0.7) for helium. The\nlatitudinal gradient is large and negative, implying significant spherical asymmetry in the\nheliospheric distribution of these particles.",
"publisher": "Department of Physics and Mathematical Physics, The University of Adelaide",
"publication_date": "1990"
},
{
"id": "authors:6h0nz-bdy87",
"collection": "authors",
"collection_id": "6h0nz-bdy87",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140508-090605066",
"type": "book_section",
"title": "Evidence for Anomalous Cosmic Ray Hydrogen",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Protheroe",
"given_name": "R. J.",
"clpid": "Protheroe-R-J"
}
],
"abstract": "The period of solar minimum activity in 1987 provided the first evidence for the\nexistence of anomalous cosmic ray (ACR) hydrogen (Christian et al. 1U88). More\nrecent data from the Voyager 1 {Vl) and Voyager 2 (V2) spacecraft and subsequent\nimproved analysis of earlier data serve to confirm the presence of ACR hydrogen.\nThis paper will cover some of these new developments in the analysis.",
"publisher": "University of Adelaide",
"publication_date": "1990"
},
{
"id": "authors:rvm1t-cee79",
"collection": "authors",
"collection_id": "rvm1t-cee79",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140714-155302359",
"type": "book_section",
"title": "Elemental Composition of the Very Local Interstellar Medium as Deduced from Observations of Anomalous Cosmic Rays",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Protheroe",
"given_name": "Raymond J.",
"clpid": "Protheroe-R-J"
}
],
"abstract": "We present a new determination of the relative abundances of the interstellar neutral\natoms CI, NI, 0 I, and Ar I. These abundances are derived from Voyager observations\nof the energy spectra of the anomalous cosmic ray- (ACR) component (He, C, N, 0, Ne, and\nAr), using a new analysis technique. We find that the abundances of NI, 0 I, and Ar I are\nin good agreement with solar system abundances, while the abundance of CI is ~1/100 of\nthe solar system value, consistent with the expectation that C is mostly ionized in the local\ninterstellar medium. As we have reported earlier, we find no evidence for charge-changing\ninteractions associated with the heliopause region.",
"publisher": "Department of Physics and Mathematical Physics, University of Adelaide",
"publication_date": "1990"
},
{
"id": "authors:tq2v1-ssb21",
"collection": "authors",
"collection_id": "tq2v1-ssb21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140708-163956095",
"type": "book_section",
"title": "Time Variation of Radial and Latitudinal Gradients of Anomalous Cosmic Ray Oxygen in the Outer Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Protheroe",
"given_name": "Raymond J.",
"clpid": "Protheroe-R-J"
}
],
"abstract": "We have used data from the Voyager I (VI), Voyager 2 (V2), and Pioneer IO (PIO)\nspacecraft to monitor the radial a.nd latitudinal gradients of anomalous cosmic ray oxygen\nin the energy range 7.1 - 17.l MeV /nuc from 1984 to 1989. We find that the latitudinal\ngradient varies from near zero value in 1984-85 to -5.5%/deg in mid-19871 returning to near\nzero value by the end of 1988. The magnitude of the latitudinal gradient is inversely correlated\nwith the radial gradient. The variations in the radial and latitudinal gradients are\ncorrelated with the tilt of the neutral sheet for tilts \u227e30 \u00b0, as expected from a sim pie model\nof particle propagation which includes curvature and gradient drifts in the large-scale\nheliospheric magnetic field.",
"publisher": "Department of Physics and Mathematical Physics, The University of Adelaide",
"publication_date": "1990"
},
{
"id": "authors:qbvfb-29521",
"collection": "authors",
"collection_id": "qbvfb-29521",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140502-091740228",
"type": "article",
"title": "Energetic Charged Particles in the Magnetosphere of Neptune",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Looper",
"given_name": "M. D.",
"clpid": "Looper-M-D"
},
{
"family_name": "Selesnick",
"given_name": "R. S.",
"clpid": "Selesnick-R-S"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Trainor",
"given_name": "J. H.",
"clpid": "Trainor-J-H"
},
{
"family_name": "Chenette",
"given_name": "D. L.",
"clpid": "Chenette-D-L"
}
],
"abstract": "The Voyager 2 cosmic ray system (CRS) measured significant fluxes of energetic [\u2273 1\nmegaelectron volt (MeV)] trapped electrons and protons in the magnetosphere of\nNeptune. The intensities are maximum near a magnetic L shell of 7, decreasing closer\nto the planet because of absorption by satellites and rings. In the region of the inner\nsatellites of Neptune, the radiation belts have a complicated structure, which provides\nsome constraints on the magnetic field geometry of the inner magnetosphere. Electron\nphase-space densities have a positive radial gradient, indicating that they diffuse inward\nfrom a source in the outer magnetosphere. Electron spectra from 1 to 5 MeV are\ngenerally well represented by power laws with indices near 6, which harden in the\nregion of peak flux to power law indices of 4 to 5. Protons have significantly lower\nfluxes than electrons throughout the magnetosphere, with large anisotropies due to\nradial intensity gradients. The radiation belts resemble those of Uranus to the extent\nallowed by the different locations of the satellites, which limit the flux at each planet.",
"doi": "10.1126/science.246.4936.1489",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "1989-12-15",
"series_number": "4936",
"volume": "246",
"issue": "4936",
"pages": "1489-1494"
},
{
"id": "authors:h465f-chr87",
"collection": "authors",
"collection_id": "h465f-chr87",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-133657111",
"type": "article",
"title": "Evidence for anomalous cosmic-ray hydrogen",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "We present evidence for the emergence of a measurable anomalous cosmic-ray hydrogen component in 1987\nwhich may account for 20%-40% of the total hydrogen flux at 60 MeV. Comparing this flux with that of\nanomalous cosmic-ray helium, we estimate that the H I/He I ratio in the very local interstellar medium is ~4,\nconsistent with determinations from solar ultraviolet backscatter measurements.",
"doi": "10.1086/185316",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "1988-11-15",
"series_number": "2",
"volume": "334",
"issue": "2",
"pages": "L77-L80"
},
{
"id": "authors:p4c06-66n86",
"collection": "authors",
"collection_id": "p4c06-66n86",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-103301989",
"type": "article",
"title": "Evidence for Anomalous Cosmic Ray Hydrogen",
"author": [
{
"family_name": "Christian",
"given_name": "E. R.",
"orcid": "0000-0003-2134-3937",
"clpid": "Christian-E-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "We present evidence for the emergence of a measurable anomalous cosmic-ray hydrogen component in 1987 which may account for 20% - 40% of the total hydrogen flux at 60 MeV. Comparing this flux with that of anomalous cosmic-ray helium, the authors estimate that the H I/He I ratio in the very local interstellar medium is ~4, consistent with determinations from solar ultraviolet backscatter measurements.",
"doi": "10.1086/185316",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "1988-11-15",
"volume": "334",
"pages": "L77-L80"
},
{
"id": "authors:c41a4-5hk66",
"collection": "authors",
"collection_id": "c41a4-5hk66",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140430-161715936",
"type": "book_section",
"title": "Composition, Gradients, and Temporal Variations of the Anomalous Cosmic-Ray Component",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Pizzo",
"given_name": "V. J.",
"clpid": "Pizzo-V-J"
},
{
"family_name": "Holzer",
"given_name": "T.",
"clpid": "Holzer-T"
},
{
"family_name": "Sime",
"given_name": "D. G.",
"clpid": "Sime-D-G"
}
],
"abstract": "Recent measurements in the outer and inner heliosphere have provided new information on the composition, spatial distribution, and temporal variations of the anomalous component. Two additional elements, carbon and argon, are now found to be enhanced, and a method has been developed to derive the abundances of the neutral gas flowing into the heliosphere. In addition, latitudinal gradients recently observed in the outer heliosphere for both the anomalous and galactic cosmic-ray components are negative, opposite to the positive latitudinal gradients reported during the 1976 period when the solar magnetic field was reversed, as expected if the latitudinal gradients are due to effects of curvature and gradient drift in the solar magnetic field. Although the radial gradient remains positive in the outer solar system, there is evidence that the gradient decreases with distance from the Sun. Finally, current 26-day variations in the flux of anomalous cosmic-ray oxygen are large and regular in 1986-1987 at Voyager 1 at ~30\u00b0 latitude but not at Voyager 2 near the ecliptic plane. We suggest that these variations may result from the combination of a latitudinal gradient with respect to magnetic latitude and the excursion of the spacecraft in latitude caused by a wavy current sheet.",
"publisher": "National Center for Atmospheric Research",
"publication_date": "1988"
},
{
"id": "authors:amfbn-5xg03",
"collection": "authors",
"collection_id": "amfbn-5xg03",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140430-091349465",
"type": "article",
"title": "Latitudinal and Radial Gradients of Anomalous and Galactic Cosmic Rays in the Outer Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "We have used measurements from instruments on Voyagers 1 and 2 and Pioneer 10 to derive simultaneous radial and latitudinal gradients of anomalous cosmic-ray oxygen during the latter part of 1985. We find that in the energy interval from 7.1-30.6 MeV/nucleon the latitudinal gradient is \u22123 to \u22124%/deg. The sign of the latitudinal gradient is opposite to that reported for the last solar cycle when the solar magnetic field polarity was reversed, as predicted by propagation models in which curvature and gradient drifts are significant. The ratios of the radial and latitudinal gradients of anomalous oxygen, anomalous helium, and galactic cosmic rays are similar, also in agreement with drift theory predictions. Based on drift theory, these observed ratios, which are near unity, lead to estimates of \u03ba/\u03b2 in the range of 3-8 \u00d7 10^(22) cm\u00b2/sec at 24.9 AU for particles with rigidities of \u223c2-3 GV.",
"doi": "10.1029/GL014i003p00174",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1987-03",
"series_number": "3",
"volume": "14",
"issue": "3",
"pages": "174-177"
},
{
"id": "authors:7mm09-8cv15",
"collection": "authors",
"collection_id": "7mm09-8cv15",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140513-101000324",
"type": "book_section",
"title": "Large-Scale Radial Gradient of Anomalous Cosmic-Ray Oxygen from 1 to ~30 AU",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Kozyarivsky",
"given_name": "V. A.",
"clpid": "Kozyarivsky-V-A"
}
],
"abstract": "The cosmic~ray instruments on IMP 8 and Voyagers 1 and 2 have been used to measure the energy spectrum and large-scale radial gradient of anomalous cosmic-ray\noxygen with -5-30 MeV/nuc for the period 1986/206-310. We find that the flux of\nanomalous oxygen at 1 AU is continuing to recover, with an average intensity that is a\nfactor of -4 lower than the 1974-78 solar minimum spectrum. The data from the three\nspacecraft are consistent with a constant radial gradient at -10 Me V /nuc of -15%/ AU\nfrom 1 to 28 AU, similar to that for the previous solar minimum period, but a factor of\n-4 higher than that for the 21- 39 AU region. These results suggest that the radial\ngradient decreases with radial distance or that there is a longitudinal gradient of\n-1%/AU. Under either assumption we find negative latitudinal gradients which, at the\nposition of Voyager 1 (-28 AU), are comparable in magnitude to the radial gradients.",
"publisher": "Proceedings of the 21st International Cosmic Ray Conference",
"publication_date": "1987"
},
{
"id": "authors:fjwtq-v7q70",
"collection": "authors",
"collection_id": "fjwtq-v7q70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140512-141917916",
"type": "book_section",
"title": "Elemental Composition of the Anomalous Cosmic-Ray Component",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Kozyarivsky",
"given_name": "V. A.",
"clpid": "Kozyarivsky-V-A"
}
],
"abstract": "We report the first definitive observations of anomalous cosmic-ray (ACR) argon and\ncarbon. Using a model for the ionization and acceleration of interstellar neutral atoms,\nwe find A CR-derived abundances for NI, Ne I, and Ar I in the very local interstellar\nmedium (VLISM) that are in excellent agreement with a compilation of solar system\nabundances, showing no evidence that significant charge-exchange processes are associated\nwith the heliopause region. The abundance of CI is nearly 2 orders of magnitude lower\nthan that of the solar system, indicating that most of the C in the VLISM is ionized. We\nfind that neither of two spectroscopically determined local interstellar components have\nneutral compositions identical to that of the ACR-derived VLISM.",
"publisher": "Proceedings of the 21st International Cosmic Ray Conference",
"publication_date": "1987"
},
{
"id": "authors:q6s7w-cky75",
"collection": "authors",
"collection_id": "q6s7w-cky75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140513-102837578",
"type": "book_section",
"title": "First Flight of a New Balloon-Borne Gamma-Ray Imaging Telescope",
"author": [
{
"family_name": "Althouse",
"given_name": "W. E.",
"clpid": "Althouse-W-E"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Finger",
"given_name": "M.",
"clpid": "Finger-M-H"
},
{
"family_name": "Palmer",
"given_name": "D. M.",
"clpid": "Palmer-D-M"
},
{
"family_name": "Prince",
"given_name": "T. A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Schindler",
"given_name": "S. M.",
"clpid": "Schindler-S-M"
},
{
"family_name": "Starr",
"given_name": "C. H.",
"clpid": "Starr-C-H"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Kozyarivsky",
"given_name": "V. A.",
"clpid": "Kozyarivsky-V-A"
}
],
"abstract": "The first flight of a new balloon-borne gamma-ray imaging payload (GRIP)\noccurred on Oct. 15 and 16, 1986 from Palestine, Texas. Observations included the\nquasar 3C273, the galactic center, and the Crab and Cygnus regions. We discuss the\ninstrument performance and present images of the Crab and Cygnus regions with 0.6\ndegree resolution over a 20 degree field of view.",
"publisher": "Proceedings of the 21st International Cosmic Ray Conference",
"publication_date": "1987"
},
{
"id": "authors:yxhjz-nd063",
"collection": "authors",
"collection_id": "yxhjz-nd063",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140513-100423829",
"type": "book_section",
"title": "Energy Spectra of Anomalous Cosmic-Ray Oxygen During 1977-1987",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Kozyarivsky",
"given_name": "V. A.",
"clpid": "Kozyarivsky-V-A"
}
],
"abstract": "We have previously reported that the energy of the peak intensity of the spectrum of\nanomalous cosmic-ray oxygen moved upwards by a factor of -2 near the time of the\nreversal of the solar magnetic field in 1980. An energy shift which persists into the next\nsolar minimum period would agree with a key prediction of a theory of the acceleration\nand propagation of the anomalous component by Jokipii. That model also predicts distinctly\ndifferent spectral shapes in the two halves of the solar magnetic cycle. Although\nwe cannot yet rule out the possibility of a long-term hysteresis in the recovery of the\nlow-rigidity particles, our spectral measurements through late 1986 agree remarkably well\nwith these predictions.",
"publisher": "Proceedings of the 21st International Cosmic Ray Conference",
"publication_date": "1987"
},
{
"id": "authors:m23f2-fa033",
"collection": "authors",
"collection_id": "m23f2-fa033",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140512-142436514",
"type": "book_section",
"title": "Radial and Latitudinal Gradients of Anomalous Cosmic-Ray Oxygen and Helium and Galactic Cosmic Rays in the Outer Heliosphere",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
}
],
"contributor": [
{
"family_name": "Kozyarivsky",
"given_name": "V. A.",
"clpid": "Kozyarivsky-V-A"
}
],
"abstract": "We have used measurements from instruments on Voyagers 1 and 2 and Pioneer 10\nto derive simultaneous latitudinal and radial gradients of anomalous cosmic-ray helium\nand oxygen and galactic cosmic rays during the latter part of 1986. We find that the\nnegative latitudinal gradients that first appeared in 1985 when Voyager 1 reached\nheliolatitudes in excess of the current sheet continue to be observed, with an increased\nmagnitude probably related to the decreasing tilt of the current sheet. The sign of this\ngradient is opposite to that reported during the last solar cycle when the solar magnetic\nfield polarity was reversed, as predicted by propagation models in which curvature and\ngradient drifts are important. Although during the 1985-1986 time period radial\ngradients in the outer heliosphere appeared to decrease, the ratios of the radial and\nlatitudinal gradients remained similar for both anomalous and galactic particles as\npredicted by drift theory. These observations indicate that the particles move inward\npreferentially at low latitudes from the heliospheric boundary during the current phase of\nthe solar cycle.",
"publisher": "Proceedings of the 21st International Cosmic Ray Conference",
"publication_date": "1987"
},
{
"id": "authors:pdfg8-sa872",
"collection": "authors",
"collection_id": "pdfg8-sa872",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140219-103051736",
"type": "article",
"title": "Solar cycle variations of anomalous ^4He as deduced by studies of cosmic ray ^3He",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"abstract": "Voyager 1 and 2 observations have been used to derive the energy spectrum of 'anomalous' cosmic ray (ACR) helium using a technique based on the separation of the isotopes of He. Previously reported observations show that the ACR oxygen spectrum underwent a change in shape following the solar magnetic field reversal in 1980; in this paper we present evidence for a corresponding change in the ACR helium spectrum. We find that the energy spectra of ACR helium and oxygen and galactic cosmic ray (GCR) ^4He and ^3He can be reproduced both before and after the field reversal using a simple solar modulation model in which the effects of curvature and gradient drifts are arbitrarily neglected.",
"doi": "10.1029/GL013i010p01043",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1986-10",
"series_number": "10",
"volume": "13",
"issue": "10",
"pages": "1043-1046"
},
{
"id": "authors:w2bcj-myj31",
"collection": "authors",
"collection_id": "w2bcj-myj31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140429-142543314",
"type": "article",
"title": "Energetic Charged Particles in the Uranian Magnetosphere",
"author": [
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Cooper",
"given_name": "J. F.",
"clpid": "Cooper-J-F"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Trainor",
"given_name": "J. H.",
"clpid": "Trainor-J-H"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "McGuire",
"given_name": "R.",
"clpid": "McGuire-R"
},
{
"family_name": "Chenette",
"given_name": "D. L.",
"clpid": "Chenette-D-L"
}
],
"abstract": "During the encounter with Uranus, the cosmic ray system on Voyager 2 measured\nsignificant fluxes of energetic electrons and protons in the regions of the planet's\nmagnetosphere where these particles could be stably trapped. The radial distribution of\nelectrons with energies of megaelectron volts is strongly modulated by the sweeping\neffects of the three major inner satellites Miranda, Ariel, and Umbriel. The phase space\ndensity gradient of these electrons indicates that they are diffusing radially inward\nfrom a source in the outer magnetosphere or magnetotail. Differences in the energy\nspectra of protons having energies of approximately 1 to 8 megaelectron volts from\ntwo different directions indicate a strong dependence on pitch angle. From the\nlocations of the absorption signatures observed in the electron flux, a centered dipole\nmodel for the magnetic field of Uranus with a tilt of 60.1 degrees has been derived, and\na rotation period of the planet of 17.4 hours has also been calculated. This model\nprovides independent confirmation of more precise determinations made by other\nVoyager experiments.",
"doi": "10.1126/science.233.4759.93",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "1986-07-04",
"series_number": "4759",
"volume": "233",
"issue": "4759",
"pages": "93-97"
},
{
"id": "authors:xfacj-h5f17",
"collection": "authors",
"collection_id": "xfacj-h5f17",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140429-131447506",
"type": "article",
"title": "Differential Measurement and Model Calculations of Cosmic-Ray Latitudinal Gradient with Respect to the Heliospheric Current Sheet",
"author": [
{
"family_name": "Christon",
"given_name": "S. P.",
"clpid": "Christon-S-P"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Behannon",
"given_name": "K. W.",
"clpid": "Behannon-K-W"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
},
{
"family_name": "Jokipii",
"given_name": "J. R.",
"clpid": "Jokipii-J-R"
},
{
"family_name": "Kota",
"given_name": "J.",
"clpid": "Kota-J"
}
],
"abstract": "Simultaneous magnetic field and charged particle measurements from the Voyager spacecraft with heliographic latitude separations of >10\u00b0 are used to investigate the distribution of \u223c1-GeV galactic cosmic ray protons with respect to the heliospheric current sheet in the outer solar system. By comparing the ratio of cosmic ray flux at Voyager 1 to that at Voyager 2 during periods of relatively quiet interplanetary conditions when the spacecraft are either both north or both south of the heliospheric current sheet, we derive an average latitude component of the gradient of the cosmic ray flux on opposite sides of the current sheet under restricted interplanetary conditions of \u22120.22\u00b10.03%/deg, equivalent to a decrease of \u223c1%/AU away from the current sheet at \u223c12 AU. Our results for these limited periods are in qualitative agreement with propagation models incorporating particle drifts.",
"doi": "10.1029/JA091iA03p02867",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "1986-03-01",
"series_number": "A3",
"volume": "91",
"issue": "A3",
"pages": "2867-2877"
},
{
"id": "authors:xpahp-5p874",
"collection": "authors",
"collection_id": "xpahp-5p874",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140429-104215151",
"type": "article",
"title": "Changes in the Energy Spectrum of Anomalous Oxygen During 1977-1985",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "We have used data from the cosmic ray experiments on the Voyager and Pioneer 10 spacecraft during the period 1977\u20131985 to measure the energy spectrum of oxygen with 4\u2013125 MeV/nucleon, with particular emphasis on the energy interval from \u223c4 to 30 MeV/nucleon, where the \"anomalous\" component of cosmic rays is dominant. This time period includes the sunspot minimum period at the beginning of solar cycle 21, the time of the solar magnetic field reversal in 1980, the maximum solar modulation period of 1981\u20131983, and part of the recovery of the solar cycle through early 1985. We find that the spectrum of anomalous oxygen changes dramatically after the middle of 1980, with the peak or plateau region of the differential spectrum shifting to a higher energy. This change does not appear to be due to the increasing radial distance of the spacecraft in this time period, nor does it appear to be simply correlated with the level of modulation. The energy shift also appears to be significantly greater in the ecliptic plane than at 24\u00b0 north latitude (the heliographic position of Voyager 1 at the end of the time period).",
"doi": "10.1029/JA091iA03p02896",
"issn": "0148-0227",
"publisher": "American Geophysical Union",
"publication": "Journal of Geophysical Research A",
"publication_date": "1986-03-01",
"series_number": "A3",
"volume": "91",
"issue": "A3",
"pages": "2896-2902"
},
{
"id": "authors:1pcaw-pmn18",
"collection": "authors",
"collection_id": "1pcaw-pmn18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-132751835",
"type": "book_section",
"title": "Radial and Latitudinal Gradients of Anomalous Oxygen During 1977-1985",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Jones",
"given_name": "F. C.",
"clpid": "Jones-F-C"
}
],
"abstract": "We find that the radial gradient of anomalous O remains constant during 1977-85\nat ~10-15%/AU although the intensity changes by more than a factor of 100.\nThese results can be used to deduce that most of the modulation of the intensities\nof these particles is occurring beyond 27 AU. We also find evidence for a latitudinal\ngradient of ~+3%/degree at low energies (7.1-10.6MeV/nuc).",
"publisher": "Goddard Space Flight Center",
"publication_date": "1985-08"
},
{
"id": "authors:kjytk-ez451",
"collection": "authors",
"collection_id": "kjytk-ez451",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-143744927",
"type": "book_section",
"title": "Differential Measurement of Cosmic-Ray Gradient with Respect to Interplanetary Current Sheet",
"author": [
{
"family_name": "Christon",
"given_name": "S. P.",
"clpid": "Christon-S-P"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Behannon",
"given_name": "K. W.",
"clpid": "Behannon-K-W"
},
{
"family_name": "Burlaga",
"given_name": "L. F.",
"orcid": "0000-0002-5569-1553",
"clpid": "Burlaga-L-F"
}
],
"contributor": [
{
"family_name": "Jones",
"given_name": "F. C.",
"clpid": "Jones-F-C"
}
],
"abstract": "Simultaneous magnetic field and charged particle measurements from the Voyager\nspacecraft at heliographic latitude separations from 10\u00b0 to 21 a are used to\ndetermine the latitude gradient of the galactic cosmic ray flux with respect to the\ninterplanetary current sheet. By comparing the ratio of cosmic ray flux at Voyager\n1 to that at Voyager 2 during periods when both spacecraft are first north\nand then south of the interplanetary current sheet, we find an estimate of the\nlatitudinal gradient with respect to the current sheet of approximately -0.15 \u00b1\n0.05 %/ deg under restricted interplanetary conditions.",
"publisher": "Goddard Space Flight Center",
"publication_date": "1985"
},
{
"id": "authors:c9jpb-qyc57",
"collection": "authors",
"collection_id": "c9jpb-qyc57",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-140747582",
"type": "book_section",
"title": "A Balloon-Borne Imaging Gamma-Ray Telescope",
"author": [
{
"family_name": "Althouse",
"given_name": "W. E.",
"clpid": "Althouse-W-E"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Finger",
"given_name": "M.",
"clpid": "Finger-M-H"
},
{
"family_name": "Prince",
"given_name": "T. A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Schindler",
"given_name": "S. M.",
"clpid": "Schindler-S-M"
},
{
"family_name": "Starr",
"given_name": "C. H.",
"clpid": "Starr-C-H"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
}
],
"contributor": [
{
"family_name": "Jones",
"given_name": "F. C.",
"clpid": "Jones-F-C"
}
],
"abstract": "This paper describes a balloon-borne coded-aperture y-ray telescope for galactic\nand extragalactic astronomy observations. The instrument, called GRIP (Gamma Ray Imaging\nPayload), is designed for measurements in the energy range from 30 keV to 5 MeV with an angular\nresolution of 0.6\u00b0 over a 20\u00b0 field of view. Distinguishing characteristics of the telescope are a\nrotating hexagonal coded-aperture mask and a thick NaI scintillation camera. Rotating hexagonal\ncoded-apertures and the development of thick scintillation cameras are discussed in Cook et\nal. [1984 and 1985, referred to as Papers I and II respectively].",
"publisher": "Goddard Space Flight Center",
"publication_date": "1985"
},
{
"id": "authors:sbe6s-seh80",
"collection": "authors",
"collection_id": "sbe6s-seh80",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-142200881",
"type": "book_section",
"title": "Changes in the Energy Spectrum of Anomalous Oxygen and Helium During 1977-1985",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Jones",
"given_name": "F. C.",
"clpid": "Jones-F-C"
}
],
"abstract": "We have used data from the cosmic-ray experiment on the Voyager spacecraft to\nmeasure the energy spectrum of anomalous O and He during the period 1977 to\n1985. We find that these spectra change dramatically after the middle of 1980,\nwith the peak or plateau region of the differential spectrum shifting to a higher\nenergy. This change appears to be related to the reversal of the solar magnetic\nfield and could imply that particle drifts are important to the acceleration or propagation\nof these particles.",
"publisher": "Goddard Space Flight Center",
"publication_date": "1985"
},
{
"id": "authors:3tca9-zv184",
"collection": "authors",
"collection_id": "3tca9-zv184",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140408-115652188",
"type": "article",
"title": "Evidence that the anomalous cosmic-ray component is singly ionized",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"abstract": "We have used data from the Cosmic Ray Subsystem on the Voyager spacecraft to measure the spectra of He, C, N, O, and Ne with 4-124 MeV per nucleon (for O) during solar minimum conditions near the end of 1977. By subtracting both a low-energy interplanetary component and the high-energy galactic component we have determined the energy spectra of the \"anomalous\" cosmic-ray species He, N, O, and Ne. The energy dependences of such spectra depend upon the charge state of the particles, their source spectra, and the rigidity dependence of the diffusion coefficient. If the source spectra at the boundary of the modulation region have similar power-law energy dependences, then the observed energy spectra indicate that the anomalous particles are singly ionized.",
"doi": "10.1086/184407",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "1984-12-15",
"series_number": "2",
"volume": "287",
"issue": "2",
"pages": "L99-L103"
},
{
"id": "authors:n600z-7tn21",
"collection": "authors",
"collection_id": "n600z-7tn21",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140421-161259173",
"type": "book_section",
"title": "Temporal Variations of the Anomalous Oxygen Component",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Neugebauer",
"given_name": "Marcia",
"clpid": "Neugebauer-M"
}
],
"abstract": "Data from the cosmic ray experiment on Voyagers 1 and 2 was used to examine anomalous oxygen in the time period from launch in 1977 to the end of 1981. Several time periods were found where large periodic (typically 26 day) temporal variations of the oxygen intensity between approximately 5 - 15 MeV/nuc are present. Variations in intensity by up to a factor of 10 are observed during these periods. Several characteristics of these variations indicate that they are not higher energy extensions of the low energy particle (approximately 1 MeV/nuc) increases found in many corotating interaction regions (CIR's). Many of these periodic temporal variations are correlated with similar, but much smaller, recurrent variations in the 75 MeV proton rate. Voyager 1 and Voyager 2 counting rates were compared to estimate the local radial gradient for both the protons and the oxygen. The proton gradients during periods of both maximum and minumum fluxes are consistent with the overall positive radial gradients reported by others from Pioneer and near-Earth observations, supporting the view that these variations are due to local modulation of a source outside the radial range of project measurements. In contrast, the oxygen gradients during periods of maximum proton flux differ in sign from those during minimum proton fluxes, suggesting that the origin of the oxygen variations is different from that of the protons.",
"publisher": "NASA",
"publication_date": "1983"
},
{
"id": "authors:maxqr-q0590",
"collection": "authors",
"collection_id": "maxqr-q0590",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140421-162004001",
"type": "book_section",
"title": "Voyager Measurements of the Energy Spectrum, Charge Composition, and Long Term Temporal Variations of the Anomalous Components in 1977-1982",
"author": [
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
}
],
"contributor": [
{
"family_name": "Neugebauer",
"given_name": "Marcia",
"clpid": "Neugebauer-M"
}
],
"abstract": "The large collecting area and wide energy range of the cosmic ray experiment on Voyager 1 and 2 was used to examine the energy spectra, charge composition, and long term temporal variations of the anomalous components in 1977-1982. Individual energy spectra are obtained for 17 separate quiet time periods during the time interval. The composite spectra of anomalous He, N, O, and Ne are obtained to a new level of precision. This includes the spectral shape and the relative abundance. Essentially, the spectral shape of N, O, and Ne appear to be similar. The ratios of anomalous N and Ne to O are found to be different from both the solar cosmic ray and galactic cosmic ray source composition. Some evidence is found for the enhancement of Ar as well. In the case of elements such as C, Mg, S, and Fe it is difficult to separate a possible lower intensity anomalous component from a quasi-steady interplanetary component that appears to be present at the lowest energies. The long term temporal variations of the anomalous He and O components were studied from 1977-82, a period from minimum to maximum in the modulation cycle. The tracking between these anomalous component intensities and the integral intensity of 75 MeV protons is striking; however, the intensity decrease of the anomalous components is much greater.",
"publisher": "NASA",
"publication_date": "1983"
},
{
"id": "authors:137cd-zdk49",
"collection": "authors",
"collection_id": "137cd-zdk49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140429-083239292",
"type": "book_section",
"title": "Short and Long Term Variations of the Anomalous Component",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Webber",
"given_name": "W. R.",
"clpid": "Webber-W-R"
}
],
"contributor": [
{
"family_name": "Durgaprasad",
"given_name": "N.",
"clpid": "Durgaprasad-N"
}
],
"abstract": "We have used data from the cosmic ray experiment (CRS) on Voyagers 1 and 2\nto examine anomalous 0 and He in the time period from launch in 1977 to\nmid-1982. We find several time periods where large periodic (typically 26 day)\ntemporal variations of 0 between - 5 -15 Me V /nuc are present, with variations\nin intensity by up to a factor of 10. On the longer term, there is a sharp drop in\nthe anomalous 0 intensity relative to the galactic co.smic ray components near\nthe middle of 1980. After the decrease we still find evidence at - 10 AU for the\npresence of anomalous 0 and He near the time of maximum modulation. Data\nfrom a larger fraction of the solar cycle will be required before it can be determined\nwhether the intensity of the anomalous component is lower in the Second\nhalf of the cycle (after the solar field reversal) than in the first half.",
"publisher": "Tata Institute of Fundamental Research",
"publication_date": "1983"
},
{
"id": "authors:ff5ns-6zt61",
"collection": "authors",
"collection_id": "ff5ns-6zt61",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140210-140754733",
"type": "article",
"title": "Energetic Charged Particles in Saturn's Magnetosphere: Voyager 2 Results",
"author": [
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
},
{
"family_name": "Chenette",
"given_name": "D. L.",
"clpid": "Chenette-D-L"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Schardt",
"given_name": "A. W.",
"clpid": "Schardt-A-W"
},
{
"family_name": "Trainor",
"given_name": "J. H.",
"clpid": "Trainor-J-H"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
}
],
"abstract": "Results from the cosmic-ray system on Voyager 2 in Saturn's magnetosphere are presented. During the inbound pass through the outer magnetosphere, the \u2265 0.43-million-electron-volt proton flux was more intense, and both the proton and electron fluxes were more variable, than previously observed. These changes are attributed to the influence on the magnetosphere of variations in the solar wind conditions. Outbound, beyond 18 Saturn radii, impulsive bursts of 0.14- to > 1.0- million-electron-volt electrons were observed. In the inner magnetosphere, the charged particle absorption signatures of Mimas, Enceladus, and Tethys are used to constrain the possible tilt and offset of Saturn's internal magnetic dipole. At \u223c 3 Saturn radii, a transient decrease was observed in the electron flux which was not due to Mimas. Characteristics of this decrease suggest the existence of additional material, perhaps another satellite, in the orbit of Mimas.",
"doi": "10.1126/science.215.4532.577",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "1982-01-29",
"series_number": "4532",
"volume": "215",
"issue": "4532",
"pages": "577-582"
},
{
"id": "authors:k3vhe-24s63",
"collection": "authors",
"collection_id": "k3vhe-24s63",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140205-155430624",
"type": "article",
"title": "Energetic Charged Particles in Saturn's Magnetosphere:\n Voyager 1 Results",
"author": [
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
},
{
"family_name": "Chenette",
"given_name": "D. L.",
"clpid": "Chenette-D-L"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Schardt",
"given_name": "A. W.",
"clpid": "Schardt-A-W"
},
{
"family_name": "Trainor",
"given_name": "J. H.",
"clpid": "Trainor-J-H"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
}
],
"abstract": "Voyager 1 provided the first look at Saturn's magnetotail and magnetosphere during relatively quiet interplanetary conditions. This report discusses the energetic particle populations of the outer magnetosphere of Saturn and absorption features associated with Titan and Rhea, and compares these observations with Pioneer 11 data of a year earlier. The trapped proton fluxes had soft spectra, represented by power laws E^\u2013\u03b3 in kinetic energy E, with \u03b3 \u223c 7 in the outer magnetosphere and \u03b3 \u223c 9 in the magnetotail. Structure associated with the magnetotial was observed as close as 10 Saturn radii (Rs) on the outbound trajectory. The proton and electron fluxes in the outer magnetosphere and in the magnetotail were variable and appeared to respond to changes in interplanetary conditions. Protons with energies \u2265 2 million electron volts had free access to the magnetosphere from interplanetary space and were not stably trapped outside \u223c 7.5 Rs.",
"doi": "10.1126/science.212.4491.231",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "1981-04-10",
"series_number": "4491",
"volume": "212",
"issue": "4491",
"pages": "231-234"
},
{
"id": "authors:vj0ph-jm616",
"collection": "authors",
"collection_id": "vj0ph-jm616",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140206-162824597",
"type": "article",
"title": "Voyager 2: Energetic Ions and Electrons in the Jovian Magnetosphere",
"author": [
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Gehrels",
"given_name": "N.",
"clpid": "Gehrels-N"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Trainor",
"given_name": "J. H.",
"clpid": "Trainor-J-H"
},
{
"family_name": "Schardt",
"given_name": "A. W.",
"clpid": "Schardt-A-W"
},
{
"family_name": "Conlon",
"given_name": "T. F.",
"clpid": "Conlon-T-F"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
}
],
"abstract": "The Voyager 2 encounter has enhanced our understanding of earlier results and provided measurements beyond 160 Jupiter radii (RJ) in the magnetotail. Significant fluxes of energetic sulfur and oxygen nuclei (4 to 15 million electron volts per nucleon) of Jovian origin were observed inside 25 RJ, and the gradient in phase space density at 12 RJ indicates that the ions are diffusing inward. A substantially longer time delay versus distance was found for proton flux maxima in the active hemisphere in the magnetotail at Jovicentric longitudes \u03bbIII, = 260\u00b0 to 320\u00b0 than in the inactive hemisphere at \u03bbIII, = 85\u00b0 to l10\u00b0. These delays can be related to the radial motion of plasma expanding into the magnetotail, and differences in the expansion speeds between the active and inactive hemispheres can produce rarefaction regions in trapped particles. It is suggested that the 10-hour modulation of interplanetary Jovian electrons may be associated with the arrival at the dawn magnetopause of a rarefaction region each planetary rotation.",
"doi": "10.1126/science.206.4421.984",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "1979-11-23",
"series_number": "4421",
"volume": "206",
"issue": "4421",
"pages": "984-987"
},
{
"id": "authors:xfk3m-wkf28",
"collection": "authors",
"collection_id": "xfk3m-wkf28",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140417-135117781",
"type": "article",
"title": "Voyager 2: Energetic Ions and Electrons in the Jovian Magnetosphere",
"author": [
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Gehrels",
"given_name": "N.",
"clpid": "Gehrels-N"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Trainor",
"given_name": "J. H.",
"clpid": "Trainor-J-H"
},
{
"family_name": "Schardt",
"given_name": "A. W.",
"clpid": "Schardt-A-W"
},
{
"family_name": "Conlon",
"given_name": "T. F.",
"clpid": "Conlon-T-F"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
}
],
"abstract": "Abstract. The Voyager 2 encounter has enhanced our understanding of earlier\nresults and provided measurements beyond 160 Jupiter radii (RJ) in the magnetotail. Significant fluxes of energetic sulfur and oxygen nuclei (4 to 15 million electron volts per nucleon) of Jovian origin were observed inside 25R^j, and the gradient in phase space density at 12 R^J indicates that the ions are diffusing inward. A substantially longer time delay versus distance was found for proton flux maxima in the active\nhemisphere in the magnetotail at Jovicentric longitudes Am = 260\u00b0 to 320\u00b0 than in the inactive hemisphere at Am = 85\u00b0 to 110\u00b0. These delays can be related to the radial motion of plasma expanding into the magnetotail, and differences in the expansion speeds between the active and inactive hemispheres can produce rarefaction regions in trapped particles. It is suggested that the JO-hour modulation of interplanetary Jovian electrons may be associated with the arrival at the dawn magnetopause of a rarefaction region each planetary rotation.",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "1979-11-13",
"series_number": "4421",
"volume": "206",
"issue": "4421",
"pages": "984-987"
},
{
"id": "authors:h254q-afn90",
"collection": "authors",
"collection_id": "h254q-afn90",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140205-163501718",
"type": "article",
"title": "Voyager 1: Energetic Ions and Electrons in the Jovian Magnetosphere",
"author": [
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
},
{
"family_name": "Cook",
"given_name": "W. R.",
"clpid": "Cook-W-R"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Gehrels",
"given_name": "N.",
"clpid": "Gehrels-N"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Trainor",
"given_name": "J. H.",
"clpid": "Trainor-J-H"
},
{
"family_name": "Schardt",
"given_name": "A. W.",
"clpid": "Schardt-A-W"
},
{
"family_name": "Conlon",
"given_name": "T.",
"clpid": "Conlon-T"
},
{
"family_name": "Lal",
"given_name": "N.",
"clpid": "Lal-N"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
}
],
"abstract": "The observations of the cosmic-ray subsystem have added significantly to our knowledge of Jupiter's magnetosphere. The most surprising result is the existence of energetic sulfur, sodium, and oxygen nuclei with energies above 7 megaelectron volts per nucleon which were found inside of Io's orbit. Also, significant fluxes of similarly energetic ions reflecting solar cosmic-ray composition were observed\nthroughout the magnetosphere beyond 11 times the radius of Jupiter. It was also found that energetic protons are enhanced by 30 to 70 percent in the active\nhemisphere. Finally, the first observations were made of the magnetospheric tail in the dawn direction out to 160 Jupiter radii.",
"doi": "10.1126/science.204.4396.1003",
"issn": "0036-8075",
"publisher": "American Association for the Advancement of Science",
"publication": "Science",
"publication_date": "1979-06-01",
"series_number": "4396",
"volume": "204",
"issue": "4396",
"pages": "1003-1007"
},
{
"id": "authors:3m3nj-nnj50",
"collection": "authors",
"collection_id": "3m3nj-nnj50",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140414-110553333",
"type": "article",
"title": "The Voyager Cosmic Ray Experiment",
"author": [
{
"family_name": "Stilwell",
"given_name": "D. E.",
"clpid": "Stilwell-D-E"
},
{
"family_name": "Davis",
"given_name": "W. D.",
"clpid": "Davis-W-D"
},
{
"family_name": "Joyce",
"given_name": "R. M.",
"clpid": "Joyce-R-M"
},
{
"family_name": "McDonald",
"given_name": "F. B.",
"clpid": "McDonald-F-B"
},
{
"family_name": "Trainor",
"given_name": "J. H.",
"clpid": "Trainor-J-H"
},
{
"family_name": "Althouse",
"given_name": "W. E.",
"clpid": "Althouse-W-E"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
}
],
"abstract": "The Voyager Cosmic Ray Experiment includes seven dE/dx-\nE telescopes to measure the energy and charge of\nparticles of 1 \u2264 Z \u2264 26 in the energy range 1-500 MeV/\nnucleon and to measure electron energy in the range\n3 \u2264 E_e \u2264 110 MeV. Isotopic composition of hydrogen\nthrough sulfur in the range up to 75 MeV/nucleon can\nalso be resolved. The electronic systems include a\ndual-gain, charge sensitive preamplifier, 4096-channel\npulse height analyzers for three parameter analysis of\nselected events, and an event type readout polling\nscheme to maximize the use of available telemetry\nspace and to enhance the occurrence of rare events in\nthe data. Details of the detector, electronic and\nmechanical design are presented.",
"doi": "10.1109/TNS.1979.4329683",
"issn": "0018-9499",
"publisher": "IEEE",
"publication": "IEEE Transactions on Nuclear Science",
"publication_date": "1979-02",
"series_number": "1",
"volume": "26",
"issue": "1",
"pages": "513-520"
},
{
"id": "authors:q892j-zpx42",
"collection": "authors",
"collection_id": "q892j-zpx42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140205-074259302",
"type": "article",
"title": "A Cosmic Ray Isotope Spectrometer",
"author": [
{
"family_name": "Althouse",
"given_name": "W. E.",
"clpid": "Althouse-W-E"
},
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Garrard",
"given_name": "T. L.",
"clpid": "Garrard-T-L"
},
{
"family_name": "Mewaldt",
"given_name": "R. A.",
"orcid": "0000-0003-2178-9111",
"clpid": "Mewaldt-R-A"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
}
],
"abstract": "We describe a new instrument to be flown on ISEE-C which is optimized to measure the isotopic composition of solar and galactic cosmic rays with ~5 to ~250 MeV/nucleon. A mass resolution of \u227e 0.3 AMU should be achieved for all elements with charge Z \u2264 30.",
"doi": "10.1109/TGE.1978.294547",
"issn": "0018-9413",
"publisher": "IEEE",
"publication": "IEEE Transactions on Geoscience Electronics",
"publication_date": "1978-07",
"series_number": "3",
"volume": "16",
"issue": "3",
"pages": "204-207"
},
{
"id": "authors:er566-t8240",
"collection": "authors",
"collection_id": "er566-t8240",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140409-090427593",
"type": "book_section",
"title": "Interstellar Electron Spectrum from the Galactic Non-Thermal Radio Emission",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
}
],
"contributor": [
{
"family_name": "Chasson",
"given_name": "R. L.",
"clpid": "Chasson-R-L"
}
],
"abstract": "A range of interstellar electron spectra at energies between\n100 MeV and 5 GeV has been derived from an analysis of the\nobserved galactic non-thermal radio spectrum and from consideration\nof the existing uncertainties in the other relevant\nphysical parameters of the galaxy. We find that for energies\nlarger than ~ 300 MeV the electron spectrum is uncertain to a\nfactor of 4 due to uncertainties in the galactic magnetic field\nstrength and the total line-of-sight emission length. The uncertainty\nin the electron spectrum increases towards lower\nenergies, exceeding a factor of 50 near 100 MeV, primarily due\nto uncertainties in the galactic parameters affecting interstellar\nradio absorption.",
"publisher": "Colorado Associated University Press",
"publication_date": "1973"
},
{
"id": "authors:k77f2-skk92",
"collection": "authors",
"collection_id": "k77f2-skk92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140409-090931878",
"type": "book_section",
"title": "Interplanetary Diffusion Coefficients for Cosmic Rays",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
}
],
"abstract": "Information on the cosmic-ray diffusion coefficient, \u03ba, derived\nfrom near-Earth observations of the solar modulation of galactic\nelectron fluxes and from the near-Earth power spectra of the\ninterplanetary magnetic field, has been used to study the\nheliocentric radial dependence of \u03ba and to derive limits on\nthe spatial extent of the solar modulation region.\n\nRepresenting \u03ba as a separable function of radius r and rigidity,\nand assuming \u03ba(r) \u221d r^n, we can place a limit on the power law\nexponent, n \u227e 1.2. The distance of the modulation boundary is\na function of n, and, e.g., for n = 0, falls into the range of\n6-25 AU.",
"publisher": "Colorado Associated University Press",
"publication_date": "1973"
},
{
"id": "authors:p5e6m-jc033",
"collection": "authors",
"collection_id": "p5e6m-jc033",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140409-090558716",
"type": "book_section",
"title": "Evidence for Primary Interstellar Cosmic-Ray Electrons",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
}
],
"abstract": "We have performed a comparative study of the absolute solar\nmodulation of cosmic-ray positrons (e^+) and electrons (e^+ + e^-).\nWe find that the interstellar electron spectrum, which is\ndescribed by a power-law slope at higher energies, must flatten\nbelow ~ 100 MeV, that a significant fraction of interstellar\ncosmic-ray electrons must originate in \"primary\" sources, and\nthat the rigidity dependence of the interplanetary cosmic-ray\ndiffusion coefficient, R^\u03b1, changes from \u03b1>O at higher rigidities\nto \u03b1 \u2248 -1 below ~ 60 MV.",
"publisher": "Colorado Associated University Press",
"publication_date": "1973"
},
{
"id": "authors:fj6r2-n8b43",
"collection": "authors",
"collection_id": "fj6r2-n8b43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140409-091427238",
"type": "book_section",
"title": "Analytic Approximations in the Study of the Solar Modulation of Electrons",
"author": [
{
"family_name": "Cummings",
"given_name": "A. C.",
"orcid": "0000-0002-3840-7696",
"clpid": "Cummings-A-C"
},
{
"family_name": "Stone",
"given_name": "E. C.",
"orcid": "0000-0002-2010-5462",
"clpid": "Stone-E-C"
},
{
"family_name": "Vogt",
"given_name": "R. E.",
"clpid": "Vogt-R-E"
}
],
"abstract": "Numerical solutions to the transport equation of galactic\ncosmic rays in the interplanetary medium have been used to\ninvestigate the applicability of commonly used approximate\nanalytic solutions for electrons (10 MeV to 10 GeV). We\nfind that for a given cosmic-ray diffusion coefficient:\n(a) the \"force-field\" approximation is in reasonable agreement\nwith the numerical solution at energies \u2273 200 MeV, but\ndeviates significantly at lower energies, depending on the\nshape of the interstellar electron spectrum, (b) the\n\"diffusion-convection\" approximation agrees generally with\nthe numerical solution within a factor of ~ 2 over the\nentire energy range.",
"publisher": "Colorado Associated University Press",
"publication_date": "1973"
}
]