[ { "id": "authors:g45by-n8m71", "collection": "authors", "collection_id": "g45by-n8m71", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150219-130839937", "type": "article", "title": "The location of Airy-0, the Mars prime meridian reference, from stereo photogrammetric processing of THEMIS IR imaging and digital elevation data", "author": [ { "family_name": "Duxbury", "given_name": "T. C.", "clpid": "Duxbury-T-C" }, { "family_name": "Christensen", "given_name": "P.", "clpid": "Christensen-P-R" }, { "family_name": "Smith", "given_name": "D. E.", "clpid": "Smith-D-E" }, { "family_name": "Neumann", "given_name": "G. A.", "clpid": "Neumann-G-A" }, { "family_name": "Kirk", "given_name": "R. L.", "clpid": "Kirk-R-L" }, { "family_name": "Caplinger", "given_name": "M. A.", "clpid": "Caplinger-M-A" }, { "family_name": "Albee", "given_name": "A. A.", "clpid": "Albee-A-L" }, { "family_name": "Seregina", "given_name": "N. V.", "clpid": "Seregina-N-V" }, { "family_name": "Neukum", "given_name": "G.", "clpid": "Neukum-G" }, { "family_name": "Archinal", "given_name": "B. A.", "clpid": "Archinal-B-A" } ], "abstract": "The small crater Airy-0 was selected from Mariner 9 images to be the reference for the Mars prime meridian. Initial analyses in the year 2000 tied Viking Orbiter and Mars Orbiter Camera images of Airy-0 to the evolving Mars Orbiter Laser Altimeter global digital terrain model to update the location of Airy-0. Based upon this tie and radiometric tracking of landers/rovers from Earth, new expressions for the Mars spin axis direction, spin rate, and prime meridian epoch value were produced to define the orientation of the Martian surface in inertial space over time. Since the Mars Global Surveyor mission and Mars Orbiter Laser Altimeter global digital terrain model were completed some time ago, a more exhaustive study has been performed to determine the accuracy of the Airy-0 location and orientation of Mars at the standard epoch. Thermal Emission Imaging System (THEMIS) IR image cubes of the Airy and Gale crater regions were tied to the global terrain grid using precision stereo photogrammetric image processing techniques. The Airy-0 location was determined to be about 0.001\u00b0 east of its predicted location using the currently defined International Astronomical Union (IAU) prime meridian location. Information on this new location and how it was derived will be provided to the NASA Mars Exploration Program Geodesy and Cartography Working Group for their assessment. This NASA group will make a recommendation to the IAU Working Group on Cartographic Coordinates and Rotational Elements to update the expression for the Mars spin axis direction, spin rate, and prime meridian location.", "doi": "10.1002/2014JE004678", "issn": "2169-9097", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research. Planets", "publication_date": "2014-12", "series_number": "12", "volume": "119", "issue": "12", "pages": "2471-2486" }, { "id": "authors:cn1rg-cjy38", "collection": "authors", "collection_id": "cn1rg-cjy38", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200505-072751563", "type": "article", "title": "The Unearthly Landscapes of Mars", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "The Red Planet is no dead planet.", "doi": "10.1038/scientificamerican0603-44", "issn": "0036-8733", "publisher": "Scientific American", "publication": "Scientific American", "publication_date": "2003-06", "series_number": "6", "volume": "288", "issue": "6", "pages": "44-53" }, { "id": "authors:sh5fz-3r212", "collection": "authors", "collection_id": "sh5fz-3r212", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130802-104030044", "type": "article", "title": "Martian rocks, minerals, and mantles", "author": [ { "family_name": "Albee", "given_name": "Arden", "clpid": "Albee-A-L" } ], "abstract": "The variable nature of Mars was first observed almost 400 years ago and modern observations began almost 40 years ago, culminating with the flotilla of spacecraft now at or heading for Mars. We now know that the atmosphere, which produced the visible variation of Mars, has also covered it with a mantle that makes difficult any detailed investigation of the rocks and minerals of Mars.", "doi": "10.1111/j.1945-5100.2002.tb00912.x", "issn": "1086-9379", "publisher": "Meteoritical Society", "publication": "Meteoritics and Planetary Science", "publication_date": "2002-05", "series_number": "S5", "volume": "37", "issue": "S5", "pages": "A9-A9" }, { "id": "authors:3v5b8-hf578", "collection": "authors", "collection_id": "3v5b8-hf578", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130802-104725010", "type": "article", "title": "Introduction to the special section: The Mars Global Surveyor mission", "author": [ { "family_name": "Albee", "given_name": "Arden", "clpid": "Albee-A-L" } ], "abstract": "Since the launch of Mars Global Surveyor (MGS) in November 1996, it has returned more information about Mars than all previous missions combined. The scientific impact of MGS has been extraordinary. In many ways we now know Mars to be a very different planet than when MGS arrived in 1997. MGS has provided daily global and high resolution images, a global topographic model better than for Earth, a corresponding gravity model, and a magnetic field model, has mapped the surface composition, and has monitored the atmosphere.", "doi": "10.1029/2001JE001511", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research E", "publication_date": "2001-10-25", "series_number": "E10", "volume": "106", "issue": "E10", "pages": "23289-23289" }, { "id": "authors:kzxhf-bn162", "collection": "authors", "collection_id": "kzxhf-bn162", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140522-104604508", "type": "article", "title": "Overview of the Mars Global Surveyor mission", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" }, { "family_name": "Arvidson", "given_name": "Raymond E.", "orcid": "0000-0002-2854-0362", "clpid": "Arvidson-Raymond-E" }, { "family_name": "Palluconi", "given_name": "Frank", "clpid": "Palluconi-Frank-D" }, { "family_name": "Thorpe", "given_name": "Thomas", "clpid": "Thorpe-Thomas" } ], "abstract": "The Mars Global Surveyor spacecraft was placed into Mars orbit on September 11, 1997, and by March 9, 1999, had slowly circularized through aerobraking to a Sun-synchronous, near-polar orbit with an average altitude of 378 km. The science payload includes the Mars Orbiter Camera, Mars Orbiter Laser Altimeter, Thermal Emission Spectrometer, Ultrastable Oscillator (for Radio Science experiments), and Magnetometer/Electron Reflectometer package. In addition, the spacecraft accelerometers and horizon sensors were used to study atmospheric dynamics during aerobraking. Observations are processed to standard products by the instrument teams and released as documented archive volumes on 6-month centers by the Planetary Data System. Significant results have been obtained from observations of the interior, surface, and atmosphere. For example, Mars does not now have an active magnetic field, although strong remanent magnetization features exist in the ancient crust. These results imply that an internal dynamo ceased operation early in geologic time. Altimetry and gravity data indicate that the crust is thickest under the south pole, thinning northward from the cratered terrain to the northern plains. Analysis of altimetry data demonstrates that Mars is \"egg-shaped\" with gravitational equipotential contours that show that channel systems in the southern highlands drained to the north, largely to the Chryse trough. A closed contour in the northern plains is consistent with the existence of a great northern ocean. Emission spectra of low-albedo regions show that basaltic rocks dominate spectral signatures on the southern highlands, whereas basaltic andesites dominate the northern lowlands. The bright regions show nondiagnostic spectra, similar to that of dust in the atmosphere. Signatures of aqueous minerals (e.g., clays, carbonates, and sulfates) are noticeably absent from the emission spectra. High spatial resolution images show that the surface has been extensively modified by wind and that layering is nearly ubiquitous, implying that a complex history of events is recorded in surface and near-surface materials. Altimetry data imply that both permanent caps are composed of water ice and dust, with seasonal covers of carbon dioxide frost. Finally, the altimetry data, coupled with thousands of atmospheric profiles, are providing new boundary conditions and dynamic controls for the generation and testing of more realistic dynamic models of the global circulation of the atmosphere.", "doi": "10.1029/2000JE001306", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research E", "publication_date": "2001-10", "series_number": "E10", "volume": "106", "issue": "E10", "pages": "23291-23316" }, { "id": "authors:121a0-fmj11", "collection": "authors", "collection_id": "121a0-fmj11", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:ALBareps00", "type": "article", "title": "Mars 2000", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "Twenty years after the Viking Mission, Mars is again being scrutinized in the light of a flood of information from spacecraft missions to Mars, the Hubble Space Telescope, and the SNC meteorites. This review provides an overview of the current understanding of Mars, especially in light of the data being returned from the Mars Global Surveyor Mission. Mars does not now have a global magnetic field, but the presence of crustal anomalies indicates that a global field existed early in Martian history. The topography, geodetic figure, and gravitational field are known to high precision. The northern hemisphere is lower and has a thinner and stronger crust than the southern hemisphere.\n\nThe global weather and the thermal structure of the atmosphere have been monitored for more than a year. Surface-atmosphere interaction has been investigated by observations of surface features, polar caps, atmospheric dust, and condensate clouds. The surface has been imaged at very high resolution and spectral measures have been obtained to quantify surface characteristics and geologic processes. Many questions remain unanswered, especially about the earliest period of Mars' history.", "doi": "10.1146/annurev.earth.28.1.281", "issn": "0084-6597", "publisher": "Annual Reviews", "publication": "Annual Review of Earth and Planetary Sciences", "publication_date": "2000-05", "volume": "28", "pages": "281-304" }, { "id": "authors:eycdb-tw822", "collection": "authors", "collection_id": "eycdb-tw822", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130802-105543692", "type": "article", "title": "Mars Global Surveyor Mission: Overview and Status", "author": [ { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Palluconi", "given_name": "F. D.", "clpid": "Palluconi-Frank-D" }, { "family_name": "Arvidson", "given_name": "R. E.", "orcid": "0000-0002-2854-0362", "clpid": "Arvidson-Raymond-E" } ], "abstract": "The Mars Global Surveyor (MGS) spacecraft achieved a 45-hour elliptical orbit at Mars on 11 September 1997 after an 11-month cruise from Earth. The mission is acquiring high-quality global observations of the martian surface and atmosphere and of its magnetic and gravitational fields. These observations will continue for one martian year.", "doi": "10.1126/science.279.5357.1671", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1998-03-13", "series_number": "5357", "volume": "279", "issue": "5357", "pages": "1671-1672" }, { "id": "authors:3369b-d7k55", "collection": "authors", "collection_id": "3369b-d7k55", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130802-134910991", "type": "article", "title": "Mars Global Surveyor: Ready for launch in November 1996", "author": [ { "family_name": "Palluconi", "given_name": "Frank D.", "clpid": "Palluconi-F-D" }, { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "The Mars Global Surveyor (MGS) spacecraft will be launched toward Mars in November 1996. This mission is the first in the NASA Mars Surveyor Program and has been under development for the past two years. In this report the status of the MGS mission, three months prior to launch, will be described along with three specific topics: aerobraking, the lander to orbiter relay and the common operations project for the Mars Surveyor Program. The Mars Global Surveyor mission is intended to accomplish a portion of the scientific objectives of the Mars Observer Mission which was lost in 1993, three days before entering Mars orbit. To meet the established objectives a low, sun-synchronous, near circular, polar-mapping orbit is required which drives the need for aerobraking before mapping begins. MGS will carry a lander to orbiter relay capability for use with the Russian 1996 lander and small probes to be dropped to the surface of Mars by the 1998 Surveyor Mission. For the Mars Surveyor Program operation of all the landers and orbiters will be conducted under a single cost constrained Mars Surveyor Operation Project.", "doi": "10.1016/S0094-5765(97)00115-X", "issn": "0094-5765", "publisher": "Elsevier", "publication": "Acta Astronautica", "publication_date": "1997-01", "series_number": "2-8", "volume": "40", "issue": "2-8", "pages": "511-516" }, { "id": "authors:bhqag-ban93", "collection": "authors", "collection_id": "bhqag-ban93", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141028-083851671", "type": "article", "title": "Mission to Mars to Collect a Storehouse of Scientific Data", "author": [ { "family_name": "Albee", "given_name": "Arden", "clpid": "Albee-A-L" } ], "abstract": "Just after Election Day, the Mars Global\nSurveyor spacecraft (Figure 1) will embark\non a journey to Mars to examine the surface\nand the seasonal variations of the atmosphere\nover an entire Mars year. Mars is an extremely\nrich mission target because the\nscientific questions it poses touch on geology,\ngeophysics, geochemistry, atmospheric\nphysics, climatology, biology, and\u2014most of\nall\u2014comparative planetology.", "doi": "10.1029/96EO00295", "issn": "0096-3941", "publisher": "American Geophysical Union", "publication": "Eos", "publication_date": "1996-11-05", "series_number": "45", "volume": "77", "issue": "45", "pages": "441-442" }, { "id": "authors:gzdt7-vcd31", "collection": "authors", "collection_id": "gzdt7-vcd31", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130802-140812019", "type": "article", "title": "Foreword [to special section on Mars Observer]", "author": [ { "family_name": "Albee", "given_name": "Arden", "clpid": "Albee-A-L" } ], "abstract": "The Mariner and Viking missions have explored Mars and have removed much of the mystery that has intrigued mankind for centuries. This knowledge allows scientists to pose complex questions about the origin, surface history, magnetic field and interior, atmosphere, and climate\nof Mars. We know enough to pose such questions, typically based on a single data set, but we do not have additional data sets with which to test these questions. Mars Observer was conceived as a mission whose observations would constitute a synergistic army of data sets that would be readily available to the global community of planetary scientists. It provides a low, Sun-synchronous, polar orbit about the planet from which the entire surface and atmosphere can be repetitively observed and mapped by remote sensing instruments for an entire Mars year. This long period of continuous observations promises a rich harvest of global and seasonal information. It will provide a basic understanding of Mars as it exists today and a framework for understanding its past. Mars Observer stands between the initial exploration of Mars and the more intensive\nExplorations, possibly involving human beings, that are only now being planned.", "doi": "10.1029/92JE00724", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research E", "publication_date": "1992-05-25", "series_number": "E5", "volume": "97", "issue": "E5", "pages": "7663-7663" }, { "id": "authors:yqeat-k6539", "collection": "authors", "collection_id": "yqeat-k6539", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130805-142011822", "type": "article", "title": "Mars Observer mission", "author": [ { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Arvidson", "given_name": "R. E.", "orcid": "0000-0002-2854-0362", "clpid": "Arvidson-Raymond-E" }, { "family_name": "Palluconi", "given_name": "F. D.", "clpid": "Palluconi-Frank-D" } ], "abstract": "The Mars Observer mission will extend the exploration and characterization of Mars by providing new and systematic measurements of the atmosphere, surface, and interior of the planet. These measurements will be made from a low-altitude polar orbiter over a period of 1 Martian year, permitting repetitive observations of the surface and of the seasonal variations of the atmosphere. The mission will be conducted in a manner that will provide new and valuable scientific data using a distributed data system that minimizes operational complexity and cost.", "doi": "10.1029/92JE00342", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research E", "publication_date": "1992-05", "series_number": "E5", "volume": "97", "issue": "E5", "pages": "7665-7680" }, { "id": "authors:jtv3p-1cq68", "collection": "authors", "collection_id": "jtv3p-1cq68", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140414-113245594", "type": "article", "title": "Mars Observer: The Next Mars Mission", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" }, { "family_name": "Palluconi", "given_name": "Frank D.", "clpid": "Palluconi-F-D" } ], "abstract": "The next mission to Mars, called Mars Observer, will be launched in September 1992. After the capture of the\nspacecraft by the planet and the adjustment into a low, Sun-synchronous, polar-mapping orbit in late 1993,\nobservations will continue for a Mars year (687 days). The scientific mission centers around global geoscience\nand climatology observations of the Mars atmosphere, surface, and interior. The seven experiments carried by\nthe spacecraft involve gamma-ray spectroscopy, magnetometry, surface and atmospheric imaging, atmospheric\nsounding, laser altimetry, gravity mapping, and thermal emission spectroscopy. All experiments contain microprocessors,\nwhich will be controlled remotely from the investigator's home institution. The long planned period\nof continuous 24 hi day observation promises a rich harvest of global and seasonal information. Mars Observer\nstands between the initial exploration of Mars and the more intensive explorations,. possibly involving human\nbeings, that are only now being planned.", "doi": "10.2514/3.26272", "issn": "0022-4650", "publisher": "American Institute of Aeronautics and Astronautics", "publication": "Journal of Spacecraft and Rockets", "publication_date": "1991-09", "series_number": "5", "volume": "28", "issue": "5", "pages": "498-500" }, { "id": "authors:04scb-0v257", "collection": "authors", "collection_id": "04scb-0v257", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131022-112714082", "type": "article", "title": "Advances in the development of encapsulants for mercuric iodide X-ray detectors", "author": [ { "family_name": "Iwanczyk", "given_name": "J. S.", "clpid": "Iwanczyk-J-S" }, { "family_name": "Wang", "given_name": "Y. J.", "clpid": "Wang-Y-J" }, { "family_name": "Bradley", "given_name": "J. G.", "clpid": "Bradley-J-G" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Schnepple", "given_name": "W. F.", "clpid": "Schnepple-W-F" } ], "abstract": "Advances in the development of protective impermeable encapsulants with high transparency to ultra-low-energy X-rays for use on HgI_2 X-ray detectors are reported. Various X-ray fluorescence spectra from coated detectors are presented. The X-ray absorption in the encapsulants has been analyzed using characteristic radiation from various elements. Results suggest that low-energy cutoffs for the detectors are not determined solely by the encapsulating coatings presently employed but are also influenced by the front electrode and surface effects, which can affect the local electric field or the surface recombination velocity. An energy resolution of 182 eV (FWHM) has been achieved for Ni L lines at 850 eV. Improved detector sensitivity to X-ray energies under 700 eV is demonstrated.", "doi": "10.1109/23.101259", "issn": "0018-9499", "publisher": "IEEE", "publication": "IEEE Transactions on Nuclear Science", "publication_date": "1990-12", "series_number": "6", "volume": "37", "issue": "6", "pages": "2214-2218" }, { "id": "authors:wctdh-a3997", "collection": "authors", "collection_id": "wctdh-a3997", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141112-102957806", "type": "article", "title": "Mars Observer's Global Mapping Mission", "author": [ { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Palluconi", "given_name": "D. F.", "clpid": "Palluconi-D-F" } ], "abstract": "The Mars Observer mission, scheduled for launch in September 1992, will provide an orbital platform at Mars from which the entire Martian surface and atmosphere will be observed beginning in late 1993. Mars Observer will extend the exploration and characterization of Mars by providing new and systematic measurements of the surface and atmosphere of the planet. These measurements will be made from a low-altitude polar orbiter over a period of one Martian year (687 Earth days), permitting repetitive observations of the surface and of the seasonal variations of the atmosphere. The mission is being designed in a manner that will provide new and valuable scientific data at a significant reduction in cost and operational complexity.", "doi": "10.1029/EO071i039p01099-01", "issn": "0096-3941", "publisher": "American Geophysical Union", "publication": "Eos", "publication_date": "1990-09-25", "series_number": "39", "volume": "71", "issue": "39", "pages": "1099-1107" }, { "id": "authors:g18hf-pcj92", "collection": "authors", "collection_id": "g18hf-pcj92", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130808-104603861", "type": "article", "title": "Practical Application of HgI_2 Detectors to a Space-Flight Scanning Electron-Microscope", "author": [ { "family_name": "Bradley", "given_name": "J. G.", "clpid": "Bradley-J-G" }, { "family_name": "Conley", "given_name": "J. M.", "clpid": "Conley-J-M" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Iwanczyk", "given_name": "J. S.", "clpid": "Iwanczyk-J-S" }, { "family_name": "Dabrowski", "given_name": "A. J.", "clpid": "Dabrowski-A-J" }, { "family_name": "Warburton", "given_name": "W. K.", "clpid": "Warburton-W-K" } ], "abstract": "Mercuric iodide X-ray detectors have been undergoing tests in a prototype scanning electron microscope system being developed for unmanned space-flight. The detector program has met with considerable success, although not all goals have yet been met. This success has been the result of carefully addressing the issues of geometric configuration in the SEM, compact packaging that includes separate thermoelectric coolers for the detector and FET, X-ray transparent hermetic encapsulation and electrical contacts, and a clean vacuum environment.", "doi": "10.1016/0168-9002(89)91383-1", "issn": "0168-9002", "publisher": "Elsevier", "publication": "Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment", "publication_date": "1989-11-01", "series_number": "2", "volume": "283", "issue": "2", "pages": "348-351" }, { "id": "authors:wt9fc-v2j80", "collection": "authors", "collection_id": "wt9fc-v2j80", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131022-110416691", "type": "article", "title": "Performance and durability of HgI_2 X-ray detectors for space missions", "author": [ { "family_name": "Iwanczyk", "given_name": "J. S.", "clpid": "Iwanczyk-J-S" }, { "family_name": "Wang", "given_name": "Y. J.", "clpid": "Wang-Y-J" }, { "family_name": "Bradley", "given_name": "J. G.", "clpid": "Bradley-J-G" }, { "family_name": "Conley", "given_name": "J. M.", "clpid": "Conley-J-M" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Economou", "given_name": "T. E.", "clpid": "Economou-T-E" } ], "abstract": "Considerable progress has been achieved in HgI_2 detector fabrication technology and amplification electronics. An energy resolution of 198 eV (full width at half maximum) has been obtained for the Mn K_\u03b1 line of 5.9 keV in a practical X-ray probe without the use of cryogenic cooling. Detectors prepared with Parylene-C encapsulation have demonstrated perfect reliability in two-year tests under high vacuum and temperature and bias cycling. Other HgI_2 detectors have been used to demonstrate proton-radiation-damage resistance to levels of 10^(12) protons/cm^2 at 10.7 MeV. It is concluded that HgI_2 detectors are suitable for the ordinary requirements of energy dispersive detectors in X-ray spectroscopy systems.", "doi": "10.1109/23.34562", "issn": "0018-9499", "publisher": "IEEE", "publication": "IEEE Transactions on Nuclear Science", "publication_date": "1989-02", "series_number": "1", "volume": "36", "issue": "1", "pages": "841-845" }, { "id": "authors:ht4w7-1gf23", "collection": "authors", "collection_id": "ht4w7-1gf23", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141217-100113797", "type": "article", "title": "The Analysis of Extraterrestrial Materials [Book Review]", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "As implied by its title, this book primarily concerns the actual analysis of extraterrestrial materials (including atmospheres and solar wind) rather than the results of such analyses. Five chapters deal with analysis of these materials in terrestrial laboratories, and six chapters describe remote analysis on spacecraft missions. Most chapters can be easily dated \u2014 they were written shortly after the mission, have undergone only sporadic updating, and are largely illustrated by copies of vu-graphs presented at National Aeronautics and Space Administration (NASA) briefings. This historical approach is quite successful in describing the original lunar receiving laboratory and instruments from specific missions. These chapters bring together good and readable descriptions of instruments from the Surveyor, Apollo, Viking, Pioneer, Venus, and especially the Soviet Lunakhod and Venera missions. The author participated in a number of the investigations involving gamma ray or X ray fluorescence spectrometry, and these sections are especially good. However, the chapters on meteorites, lunar samples, cosmochronology, and reflectance spectroscopy are too dated and should have been completely rewritten to properly convey current research and understanding.", "doi": "10.1029/88EO00227", "issn": "0096-3941", "publisher": "American Geophysical Union", "publication": "Eos", "publication_date": "1988-06-21", "series_number": "25", "volume": "69", "issue": "25", "pages": "670" }, { "id": "authors:vpc3x-5c664", "collection": "authors", "collection_id": "vpc3x-5c664", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130805-150254709", "type": "article", "title": "Scanning Electron-Microscopes and Other Beam Instruments for Spaceflight", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "SEMPA (Scanning Electron Microscope and\nParticle Analyser) is-a newly developed\nspacecraft instrument, miniaturized from\nfamiliar laboratory instruments for NASA's\nComet Rendezvous/Asteroid Flyby mission in the\n'90's. SEMPA will determine elemental\ncomposition, shape, morphology, and mineralogy\nof individual dust particles and charaterize\nthe flux. Spaceflight requirements demanded\ntradeoffs against current instrument\nperformance and design concepts to adopt to the\nspace environment, minimize weight and power\nconsumption, and increase the maintenance-free\nlifetime.\nOther instruments that utilize in-site\nexcitation of \"rocky\" samples are being\ndesigned by U.S., Soviet, and European\nscientists for future space missions. Under\nconsideration is excitation with ion beams,\nlaser beams, white light, pulsed neutron\ngenerators, x-ray generators, and particle\naccelerations.", "doi": "10.1002/jemt.1060070212", "issn": "0741-0581", "publisher": "Wiley", "publication": "Journal of Electron Microscopy Technique", "publication_date": "1987-10", "series_number": "2", "volume": "7", "issue": "2", "pages": "137-137" }, { "id": "authors:060sv-8qj58", "collection": "authors", "collection_id": "060sv-8qj58", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230105-204018447", "type": "article", "title": "Caltech Applauds Crafoord Laureate", "author": [ { "family_name": "Kamb", "given_name": "Barclay", "clpid": "Kamb-B" }, { "family_name": "Vogt", "given_name": "Rochus", "clpid": "Vogt-R-E" }, { "family_name": "Wyllie", "given_name": "Peter", "clpid": "Wyllie-P-J" }, { "family_name": "Goldberger", "given_name": "Marvin", "clpid": "Goldberger-M-L" }, { "family_name": "Fowler", "given_name": "Willy", "clpid": "Fowler-W-A" }, { "family_name": "Greenstein", "given_name": "Jesse", "clpid": "Greenstein-J-L" }, { "family_name": "Sharp", "given_name": "Bob", "clpid": "Sharp-R-P" }, { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "On November 20 friends and colleagues of Gerald J. Wasserburg gathered at Caltech's Athenaeum to honor him as recipient of the 1986 Crafoord Prize. Awarded annually by the Royal Swedish Academy of Sciences, the prize for work in mathematics, astronomy, geosciences, or biosciences is one of the scientific community's most prestigious honors. The award cited Wasserburg, the John D. MacArthur Professor of Geology and Geophysics, for his \"major impact on our knowledge of the universe, focusing on the origins and history of the solar system and its component bodies. His work has established a time scale for the development of the early solar system and the formation of the planets, the moons, and the meteorites.\"", "issn": "0013-7812", "publisher": "California Institute of Technology", "publication": "Engineering and Science", "publication_date": "1987-01", "series_number": "3", "volume": "50", "issue": "3", "pages": "14-19" }, { "id": "authors:0g02j-egk51", "collection": "authors", "collection_id": "0g02j-egk51", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131008-143821891", "type": "article", "title": "Low Energy X-Ray Spectra Measured with a Mercuric Iodide Energy Dispersive Spectrometer in a Scanning Electron Microscope", "author": [ { "family_name": "Iwanczyk", "given_name": "J. S.", "clpid": "Iwanczyk-J-S" }, { "family_name": "Dabrowski", "given_name": "A. J.", "clpid": "Dabrowski-A-J" }, { "family_name": "Huth", "given_name": "G. C.", "clpid": "Huth-G-C" }, { "family_name": "Bradley", "given_name": "J. G.", "clpid": "Bradley-J-G" }, { "family_name": "Conley", "given_name": "J. M.", "clpid": "Conley-J-M" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" } ], "abstract": "A mercuric iodide energy dispersive x-ray\nspectrometer, with Peltier cooling provided for the\ndetector and input field effect transistor, has been\ndeveloped and tested in a scanning electron microscope.\nX-ray spectra were obtained with the 15 keV electron\nbeam. An energy resolution of 225 eV (FWHM) for Mn-K\u03b1\nat 5.9 keV and 195 eV (FWHM) for Mg-K line at 1.25 keV\nhas been measured. Overall system noise level was 175\neV (FWHM). The detector system characterization with a\ncarbon target demonstrated good energy sensitivity at\nlow energies and lack of significant spectral artifacts\nat higher energies.", "doi": "10.1109/TNS.1986.4337118", "issn": "0018-9499", "publisher": "IEEE Transactions on Nuclear Science", "publication": "IEEE Transactions on Nuclear Science", "publication_date": "1986-02", "series_number": "1", "volume": "33", "issue": "1", "pages": "355-358" }, { "id": "authors:e7q3g-86883", "collection": "authors", "collection_id": "e7q3g-86883", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150211-091223549", "type": "article", "title": "Kimberlites I: Kimberlites and Related Rocks. Kimberlites II: The Mantle and Crust-Mantle Relationships [Book Review]", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "These volumes open with a tribute to academician Vladimir Stepanovich Sobolev, who died several days before the opening of the Third International Kimberlite Conference at Clermont Ferrand, France. V.S. Sobolev made major contributions to the field of kimberlite and upper mantle petrology throughout his lifetime and did much to spark the renaissance in this field that led to these conferences.", "doi": "10.1029/EO066i007p00063", "issn": "0096-3941", "publisher": "American Geophysical Union", "publication": "Eos", "publication_date": "1985-02-12", "series_number": "7", "volume": "66", "issue": "7", "pages": "63" }, { "id": "authors:ahmgx-9rf22", "collection": "authors", "collection_id": "ahmgx-9rf22", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140414-105654946", "type": "article", "title": "Distribution of Ordovician and Devonian metamorphism in mafic and pelitic schists from northern Vermont", "author": [ { "family_name": "Laird", "given_name": "Jo", "clpid": "Laird-J" }, { "family_name": "Lanphere", "given_name": "Marvin A.", "clpid": "Lanphere-M-A" }, { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "^(40)Ar/^(39) Ar range from 471 to 439 my and confirm that Ordovician metamorphism is recorded from the Canadian border south to the Precambrian core of the Green Mountain Anticlinorium (GMA). Medium-high pressure (P) facies series metamorphism in the north and medium-P metamorphism to the south. Similar metamorphic ages and compatible estimates of T and P indicate mafic and pelitic rocks were metamorphosed together. Medium-P Devonian metamorphism has overprinted the Ordovician metamorphism in northern Vermont east and probably west of the GMA axis, resulting in conventional K/Ar, ^(40)Ar/^(39)Ar total fusion and plateau ages of 386 to 355 my on muscovite, biotite, and amphibole.\n--Modified journal abstract.", "doi": "10.2475/ajs.284.4-5.376", "issn": "0002-9599", "publisher": "American Journal of Science", "publication": "American Journal of Science", "publication_date": "1984-05", "series_number": "4-5", "volume": "284", "issue": "4-5", "pages": "376-413" }, { "id": "authors:jg297-sam86", "collection": "authors", "collection_id": "jg297-sam86", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141212-131937251", "type": "article", "title": "Scanning Electron Microscopy and X-Ray Microanalysis [Book Review]", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "This outstanding volume has managed the nearly impossible task of combining the expertise of all six authors in a lucid and homogeneous style of writing. Subtitled 'A Text for Biologists, Material Scientists and Geologists,' the book has evolved from a short course taught each summer at Lehigh University.\n\nThe book provides a basic knowledge of (1) the electron optics for these instruments a nd their controls, (2) the characteristics of the electron beam-sample interactions, (3) image formation and interpretation, (4) X ray spectrometry and quantitative X ray microanalysis with separate detailed sections on wavelength dispersive and energy dispersive techniques, and (5) specimen preparation, especially for biological materials.", "doi": "10.1029/EO063i047p01188", "issn": "0096-3941", "publisher": "American Geophysical Union", "publication": "Eos", "publication_date": "1982-11-23", "series_number": "47", "volume": "63", "issue": "47", "pages": "1188" }, { "id": "authors:xh6nh-rvq92", "collection": "authors", "collection_id": "xh6nh-rvq92", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140414-111513915", "type": "article", "title": "Crystallization Paths of Leucite-Bearing Lavas: Examples from Italy", "author": [ { "family_name": "Baldridge", "given_name": "W. Scott", "clpid": "Baldbridge-W-Scott" }, { "family_name": "Carmichael", "given_name": "I. S. E.", "clpid": "Carmichael-Ian-S-E" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" } ], "abstract": "The salic phases found in leucite-basanites, -trachytes, and -phonolites may be used to portray crystallization in the system NaAlSiO_4-KAlSiO_4-CaAl_2Si_2O_8-SiO_2, the phonolite pentahedron. Only two lavas have been found that contain the assemblage leucite-nepheline-plagioclase-sanidine and liquid, a natural pseudo-invariant assemblage (at 900\u00b0 C\u00b1100) equivalent to the isobaric invariant point of the four component system. The diversity of phases in this group of lavas illustrates the role of halogens in controlling their crystallization paths. Thus the presence of F in the leucite-basanites has stabilized magnesian biotite and suppressed sanidine, as has been found in other basanitic lavas (Brown and Carmichael 1969). The presence of Cl in these same lavas has induced the crystallization of sodalite, which takes the place of nepheline in the groundmass. However in the leucite-trachytes, biotite has suppressed olivine and coexists with sanidine and leucite. The presence of S may produce ha\u00fcyne at the expense of nepheline, and in general sulphate minerals, which include apatite, have the role in lavas of low silica activity that pyrrhotite plays in liquids of high silica activity. Both pyroxenes and titaniferous magnetites in this suite of lavas are very aluminous. Groundmass crystals of pyroxene may have one-fifth of Si replaced by Al. Other phases which occur occasionally are melanite garnet and a potassium-rich hastingsite, but neither ilmenite nor a sulphide mineral has been found. Phenocryst equilibration temperatures, derived from olivine and Sr-rich plagioclase, are generally in the range from 1,050\u00b0 C to 1,150\u00b0 C. The high content of incompatible elements (e.g., K, Ba, Rb, F, Sr, P) in these lavas suggests that they represent a small liquid fraction from a mantle source which possibly contains phlogopite.", "doi": "10.1007/BF00375459", "issn": "0010-7999", "publisher": "Springer", "publication": "Contributions to Mineralogy and Petrology", "publication_date": "1981-05", "series_number": "3", "volume": "76", "issue": "3", "pages": "321-335" }, { "id": "authors:hdhbg-ve533", "collection": "authors", "collection_id": "hdhbg-ve533", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140414-102536185", "type": "article", "title": "Pressure, temperature, and time indicators in mafic schist; their application to reconstructing the polymetamorphic history of Vermont", "author": [ { "family_name": "Laird", "given_name": "Jo", "clpid": "Laird-J" }, { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "Mineral chemistry and overgrowth relationships in mafic schist from Vermont are shown to be sensitive indicators of pressure, temperature, and relative time and to be good chronicles of the Paleozoic history of this polymetamorphic terrane. Within the common assemblage, amphibole + chlorite + epidote + plagioclase +quartz+ Ti-phase \u00b1 carbonate \u00b1 K-mica \u00b1 Fe^(3+)-oxide, electron microprobe analyses show that increasing metamorphic grade (as defined by intercalated pelitic schist) is recorded by an increase in the edenite, glaucophane, and tschermakite contents of\namphibole, in the anorthite content of plagioclase, and in the substitution of (Al^(VI),F^(2+), Ti), Al^(IV) for (Fe^(2+), Mg, Mn), Si in biotite, chlorite, and muscovite. With increasing pressure the glaucophane component of amphibole increases. For medium-pressure metamorphism the albite-oligoclase gap is in the garnet zone, where amphibole has between 1.2 and 1.8 formula proportion Al^(IV) and (Al^(VI) + Fe^(3+) + Ti + Cr). This gap is below the garnet isograd in low-pressure mafic schist where Al^(IV) and (Al^(VI) + Fe^(3+) + Ti + Cr) in the amphibole are both less than 0.6. Mineral growth periods observed are characterized by metamorphic grade and facies series and are assigned to two Ordovician (Taconic) and two Devonian (Acadian) events. Silurian-Devonian mafic schist in northeastern Vermont records two periods of low-pressure, Devonian metamorphism. These events are expressed by medium-pressure and low-pressure metamorphism in the Cambrian and Ordovician rocks to the west and south. In the pre-Silurian rocks high-pressure and medium-pressure metamorphism is assigned to the Ordovician. The observed high-pressure metamorphism is confined to a 110 by 40 km area along the Green Mountain anticlinorium axis in north-central Vermont.", "doi": "10.2475/ajs.281.2.127", "issn": "0002-9599", "publisher": "American Journal of Science", "publication": "American Journal of Science", "publication_date": "1981-02-01", "series_number": "2", "volume": "281", "issue": "2", "pages": "127-175" }, { "id": "authors:djmwh-r4n85", "collection": "authors", "collection_id": "djmwh-r4n85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140414-093459837", "type": "article", "title": "High-pressure metamorphism in mafic schist from northern Vermont", "author": [ { "family_name": "Laird", "given_name": "Jo", "clpid": "Laird-J" }, { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "The only confirmed occurrence of glaucophane and omphacite in the Appalachian Mountains of New England is in mafic schist from Tillotson Peak (44\u00b048', 72\u00b033'), north-central Vermont. Mineral assemblages observed, all with epidote\n+ sphene \u00b1 magnetite \u00b1 phengitic muscovite \u00b1 carbonate (calcite or dolomite) \u00b1 apatite \u00b1 sulfide, are: (1) actinolite + glaucophane + chlorite + garnet + quartz, (2)\nactinolite + glaucophane + chlorite + albite + garnet, (3) actinolite + glaucophane + omphacite + garnet, (4) glaucophane + chlorite + garnet+ quartz, (5) glaucophane\n+ omphacite + quartz, (6) albite + glaucophane + chlorite + quartz, and (7) albite + paragonite + chlorite + quartz. Electron microprobe investigations show that plagioclase, chlorite, sphene, white mica, carbonate, and magnetite grains are relatively homogeneous. However, amphibole, pyroxene, epidote, and garnet grains are zoned, indicating incomplete equilibration and changing physical conditions during metamorphism. Glaucophane in assemblage (6) has the general formula (rim composition): \u25a1 (Na_(1.9^(M4)Ca_(0.1)) (Mg_(1.8Fe_(1.2)^(2+)Al_(1.0)^(VI)Fe_(0.3)^(3+)) (Si_(7.9)Al_(0.1)^(IV)) O_(22) (OH)_(2\u2022) Glaucophane in assemblages (1) to (5) is somewhat poorer in the glaucophane endmember and richer in actinolite. Ca-rich amphibole grains are zoned extensively with barroisite cores and actinolite rims. Omphacite grains in assemblages (3) and (5) have the general formula (rim composition) (Na_(0.5)Ca_(0.5)) (Mg_(0.4)Fe_(0.1)^(2+)Al_(0.4)^(VI)Fe_(0.1)^(3+)) Si_2O_6.\nIn spite of the significant zoning, the partitioning of elements among the minerals at their grain margins suggests that all seven assemblages above may coexist at the same physical conditions of metamorphism in mafic rocks with a relatively small range in bulk composition. Correlation of mineral compositions and assemblages with mineral stability data suggests high-pressure facies series metamorphism at about 9 \u00b1 2 kb and 450 \u00b1 100\u00b0C with P_(h2O) \u2248 P_(Total). It is proposed that the metamorphism occurred during the Ordovician.", "doi": "10.2475/ajs.281.2.97", "issn": "0002-9599", "publisher": "American Journal of Science", "publication": "American Journal of Science", "publication_date": "1981-02-01", "series_number": "2", "volume": "281", "issue": "2", "pages": "97-126" }, { "id": "authors:wst96-fmq72", "collection": "authors", "collection_id": "wst96-fmq72", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131015-145647213", "type": "article", "title": "Stratigraphy, structure, and metamorphism in the central Panamint Mountains (Telescope Peak quadrangle), Death Valley area, California: Summary", "author": [ { "family_name": "Labotka", "given_name": "Theodore C.", "clpid": "Labotka-T-C" }, { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" }, { "family_name": "Lanphere", "given_name": "Marvin A.", "clpid": "Lanphere-M-A" }, { "family_name": "McDowell", "given_name": "S. Douglas", "clpid": "McDowell-S-D" } ], "abstract": "The Telescope Peak quadrangle is located in the central Panamint Mountains, which form the western boundary of the central\npart of Death Valley, California. The central Panamint Mountains are composed of lower Precambrian gneiss and schist and upper\nPrecambrian sedimentary rocks. These rocks were metamorphosed during late Mesozoic time and deformed during late Mesozoic and\nCenozoic time. The stratigraphy of the upper Precambrian rocks indicates a tectonically active depositional environment during the\ninitiation of the Cordilleran geosyncline; the petrology of the metamorphic rocks indicates that the metamorphism occurred\nalong a gradient with a low dp/dT; and the structure suggests an evolution from a compressional to an extensional tectonic regime\nduring late Mesozoic and Tertiary time. \n\nThis report summarizes the results of geologic mapping in the Telescope Peak quadrangle, and Figure 1 is a generalized version of the geologic map of the Telescope Peak 15' quadrangle by Albee, Labotka, Lanphere, and McDowell (1980). A more complete discussion of the geology occurs in Part II of this article.", "doi": "10.1130/0016-7606(1980)91<125:SSAMIT>2.0.CO;2", "issn": "0016-7606", "publisher": "Geological Society of America", "publication": "Geological Society of America Bulletin", "publication_date": "1980-03", "series_number": "3", "volume": "91", "issue": "3", "pages": "125-129" }, { "id": "authors:88w4p-0kh46", "collection": "authors", "collection_id": "88w4p-0kh46", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131015-154255329", "type": "article", "title": "Silica solid solution and zoning in natural plagioclase", "author": [ { "family_name": "Beaty", "given_name": "David W.", "clpid": "Beaty-D-W" }, { "family_name": "Albee", "given_name": "Arden", "clpid": "Albee-A-L" } ], "abstract": "Microprobe analyses of plagioclase from some lunar basalts have anomalous stoichiometry\nas compared to terrestrial feldspars. The anomaly indicates the presence of the \"excess silica\"\nsubstitution, [ ]Si_4O_8. This coupled substitution leaves a vacancy in the feldspar lattice and\nis effectively SiO_2, dissolved in the feldspar. Detailed study indicates that core-rim [ ]Si_4O_8,\nzoning is a common phenomenon in plagioclase from lunar basalts. Anorthite-albite zoning\nis also typically present, so plots of [ ]Si_4O_8 as a function of anorthite content provide a convenient\nmeasure of the [ ]Si_4O_8 variations present. Most lunar basaltic plagioclase shows a monotonic increase in [ ]Si_4O_8 with albite content, typically ranging from 0 mole percent\n[ ]Si_4O_8 in the cores to 5-7 percent in the rims. This zoning is produced by two cooperating\nprocesses: a falling temperature of formation, and growth from a progressively siliceous liquid.\nIn addition, rapid growth and delayed nucleation of plagioclase and silica phase appear\nto be important to the disequilibrium incorporation of [ ]Si_4O_8.\n\n\nBy contrast, plagioclase from a wide variety of terrestrial occurrences lacks [ ]Si_4O_8. The\nAbsence of [ ]Si_4O_8 in many terrestrial igneous plagioclases is primarily related to the presence of H_2O, which decreases the liquidus temperatures relative to those in lunar rocks. Terrestrial\nbasalts which have comparable crystallization temperatures to their lunar counterparts\nlack [ ]Si_4O_8 in part because of an absence of strong in situ differentiation. In addition,\nplagioclase typically crystallizes prior to pyroxene (the reverse of the mare basalts), so kinetic\neffects have a reduced role. If a melt is in equilibrium with cristobalite (or tridymite or\nquartz), the silica activity is buffered, and the [ ]Si_4O_8, content of the plagioclase is directly\nrelated to the temperature. [ ]Si_4O_8, incorporation, however, is typically not an equilibrium\nprocess, so there is little hope of using it directly as a geothermometer.", "issn": "0003-004X", "publisher": "Mineralogical Society of America", "publication": "American Mineralogist", "publication_date": "1980-01", "series_number": "1-2", "volume": "65", "issue": "1-2", "pages": "63-74" }, { "id": "authors:n0qy1-b6122", "collection": "authors", "collection_id": "n0qy1-b6122", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131118-132153939", "type": "article", "title": "Serpentinization of the Belvidere Mountain ultramafic body, Vermont; mass balance and reaction at the metasomatic front", "author": [ { "family_name": "Labotka", "given_name": "Theodore C.", "clpid": "Labotka-T-C" }, { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "Chrysotile-asbestos veins that cut the relatively unaltered dunite core of the ultramafic body at Belvidere Mountain, Vermont, are bordered by symmetrical serpentinite zones composed of antigorite, magnetite and brucite. This serpentinite is separated from the dunite host by a sharp reaction front, and the modal mineralogy and mineral chemistry of the two rock-types adjacent to the front\nwere determined in order to characterize the serpentinization reaction. A mass balance of bulk chemistry indicates that the serpentinite formed by the addition of SiO_2, and H_2O, loss of H_2, and without net loss of magnesium. A reaction that most closely represents the serpentinization front is: 100 olivine + 25 SiO_2 + 129 H_2O = 31 antigorite + 4 magnetite + 4 H_2. The presence of\nessentially monomineralic zones suggests that SiO_2, H_2O and H_2 activities were externally controlled. Local concentrations of brucite indicate that the activities of those components were locally appropriate for the stability of brucite.", "issn": "0008-4476", "publisher": "Mineralogical Association of Canada", "publication": "Canadian Mineralogist", "publication_date": "1979-11", "series_number": "4", "volume": "17", "issue": "4", "pages": "831-845" }, { "id": "authors:wt6t3-y9j63", "collection": "authors", "collection_id": "wt6t3-y9j63", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130806-152922789", "type": "article", "title": "Titanium and Aluminum in Biotite From High-Grade Archaean Gneisses, Lang\u00f8, West Greenland", "author": [ { "family_name": "Dymek", "given_name": "R. F.", "clpid": "Dymek-R-F" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" } ], "abstract": "Biotite grains from a variety of gneiss types were analyzed by electron microprobe techniques\nfor Na, Mg, Al, Si, K, Ca, Ti, Mn, Fe, Zn, F & Cl. TiO_2- and Al_2O_3-contents range continuously\nfrom < 0.1 to 6.0 and 13.9 to 20.6 wt % respectively. Most occur with ilmenite, but a few coexist\nwith rutile. Biotite in pyribolite contains the least Al, and that in Kfeld-sill gneiss\ncontains the most, suggesting that Al-content of biotite is related to the bulk composition of the\nhost rock. For a given rock type, Ti in biotite tends to decrease as Mg/Fe and Al increase.", "doi": "10.1029/EO058i006p00366", "issn": "0002-8606", "publisher": "American Geophysical Union", "publication": "Transactions - American Geophysical Union", "publication_date": "1977-06", "series_number": "6", "volume": "58", "issue": "6", "pages": "525-525" }, { "id": "authors:cg5fm-86788", "collection": "authors", "collection_id": "cg5fm-86788", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131021-154533262", "type": "article", "title": "Petrography of isotopically-dated clasts in the Kapoeta howardite and petrologic constraints on the evolution of its parent body", "author": [ { "family_name": "Dymek", "given_name": "R. F.", "clpid": "Dymek-R-F" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Chodos", "given_name": "A. A.", "clpid": "Chodos-A-A" }, { "family_name": "Wasserburg", "given_name": "G. J.", "orcid": "0000-0002-7957-8029", "clpid": "Wasserburg-G-J" } ], "abstract": "Detailed mineralogic and petrographic data are presented for four isotopically-dated basaltic rock fragments separated from the howardite Kapoeta. Clasts C and \u03c1 have been dated at ~4.55 AE and ~ 4.60 AE respectively, and Clast \u03c1 contains ^(244)Pu and ^(129)I decay products. These are both igneous rocks that preserve all the features of their original crystallization from a melt. They thus provide good evidence that the Kapoeta parent body produced basaltic magmas shortly after its formation (< 100 m.y.). Clast A has yielded a Rb-Sr age of ~ 3.89 AE and a similar ^(40)Ar/^(39)Ar\nage. This sample is extensively recrystallized, and we interpret the ages as a time of recrystallization, and not the time of original crystallization from a melt. Clast B has yielded a Rb-Sr age of ~ 3.63 AE, and an ^(40)Ar/^(39)Ar age of \u2a86 4.50 AE. This sample is moderately recrystallized, and the Rb-Sr age probably indicates a time of recrystallization, whereas the ^(40)Ar/^(39)Ar age more closely approaches the time of crystallization from a melt. Thus, there is no clearcut evidence for 'young' magmatism on the Kapoeta parent body.\n\nKapoeta is a 'regolith' meteorite, and mineral-chemical and petrographic data were obtained for numerous other rock and mineral fragments in order to characterize the surface and near-surface materials on its parent body. Rock clasts can be grouped into two broad lithologic types on the basis of modal mineralogy\u2014basaltic (pyroxene- and plagioclase-bearing) and pyroxenitic (pyroxenebearing). Variations in the compositions of pyroxenes in rock and mineral clasts are similar to those in terrestrial mafic plutons such as the Skaergaard, and indicate the existence of a continuous range in rock compositions from Mg-rich orthopyroxenites to very iron-rich basalts. The FeO and MnO contents of all pyroxenes in Kapoeta fall near a line with FeO/MnO ~ 35, suggesting that the source rocks are fundamentally related. We interpret these observations to indicate that the Kapoeta meteorite represents the comminuted remains of differentiated igneous complexes together with 'primary' undifferentiated basaltic rocks. The presently available isotopic data are compatible with the interpretation that this magmatism is related to primary differentiation of the Kapoeta parent body. In addition, our observations preclude the interpretation that the Kapoeta meteorite is a simple mixture of eucrites and diogenites.\n\nThe FeO/MnO value in lunar pyroxenes (~60) is distinct from that of the pyroxenes in Kapoeta. Anorthositic rocks were not observed in Kapoeta, suggesting that plagioclase was not important in the evolution of the Kapoeta parent body, in contrast to the Moon. Both objects appear to have originated in chemically-distinct portions of the solar system, and to have undergone differentiation on different time scales involving differing materials.", "doi": "10.1016/0016-7037(76)90053-3", "issn": "0016-7037", "publisher": "Elsevier", "publication": "Geochimica et Cosmochimica Acta", "publication_date": "1976-09", "series_number": "9", "volume": "40", "issue": "9", "pages": "1115-1130" }, { "id": "authors:hmaqk-5at25", "collection": "authors", "collection_id": "hmaqk-5at25", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130806-100459556", "type": "article", "title": "A review of lunar sample studies and their application to studies of the terrestrial planets", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "During the last half decade, hundreds of scientists from many countries have been studying the samples, photographs, and instrumental data returned from the moon by the Apollo and Luna programs. These studies have placed significant limits on chemical, petrologic, and physical parameters, on the time of many events, and on the rate of many processes and are giving greater insight into the natural processes that formed the moon and shaped its surface. Increasingly, it is being recognized that very similar processes governed the origin and evolution of planetary bodies throughout the solar system. Spacecraft have extended our sensors to all the terrestrial planets, and the insights gained from Apollo dominate our interpretation of the photographic and instrumental data returned from these bodies.", "doi": "10.1029/RG013i003p00419", "issn": "0034-6853", "publisher": "American Geophysical Union", "publication": "Reviews of Geophysics and Space Physics", "publication_date": "1975-07", "series_number": "3", "volume": "13", "issue": "3", "pages": "419-422" }, { "id": "authors:bfc0a-dx324", "collection": "authors", "collection_id": "bfc0a-dx324", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180313-073633736", "type": "article", "title": "Constrained least-squares analysis of petrologic problems with an application to lunar sample 12040", "author": [ { "family_name": "Reid", "given_name": "M. J.", "orcid": "0000-0001-7223-754X", "clpid": "Reid-M-J" }, { "family_name": "Gancarz", "given_name": "A. J.", "clpid": "Gancarz-A-J" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" } ], "abstract": "Many petrologic problems, which may be expressed as a set of linear equations, have been solved by least-squares analysis. In many cases insufficient attention has been paid to the physical conditions of the model resulting in incorrect application of the method. This paper presents a systematic treatment of the application of least-squares analysis to petrologic problems including the direct utilization of physical constraints and weighting factors in the problem, and the assessment of uncertainties in the solution. As an example, least-squares analysis is used to examine, in detail, the mass balance equations for lunar rock 12040 and to determine the consistency of the available analytical data.", "doi": "10.1016/0012-821X(73)90212-4", "issn": "0012-821X", "publisher": "Elsevier", "publication": "Earth and Planetary Science Letters", "publication_date": "1973-01", "series_number": "2", "volume": "17", "issue": "2", "pages": "433-445" }, { "id": "authors:pajwe-h2643", "collection": "authors", "collection_id": "pajwe-h2643", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180307-083914238", "type": "article", "title": "Comparative petrology of Apollo 16 sample 68415 and Apollo 14 samples 14276 and 14310", "author": [ { "family_name": "Gancarz", "given_name": "A. J.", "clpid": "Gancarz-A-J" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Chodos", "given_name": "A. A.", "clpid": "Chodos-A-A" } ], "abstract": "Petrographic and electron microprobe studies of Apollo 16 igneous rock 68415 and Apollo 14 rocks 14276 and 14310 show that all three samples differ from the mare basalts and are characterized by plagioclase as the first liquidus phase and by the abundance of plagioclase which is in part cumulate in origin. Major and minor element abundances and isotopic data prohibit the derivation of rocks like any of these samples from one another by magmatic fractionation during their crystallization. They could have originated by partial melting of an old, more Al-rich source material without isotopic equilibration with the residuum, by complete melting of three independent sources, or by contamination with old radiogenic material. The existence of such feldspathic basalts indicates that the generation of Al-rich magmas may have been an important and widespread lunar process.", "doi": "10.1016/0012-821X(72)90150-1", "issn": "0012-821X", "publisher": "Elsevier", "publication": "Earth and Planetary Science Letters", "publication_date": "1972-11", "series_number": "3", "volume": "16", "issue": "3", "pages": "307-330" }, { "id": "authors:pwa0y-hwm50", "collection": "authors", "collection_id": "pwa0y-hwm50", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180228-105651836", "type": "article", "title": "Mineralogy, petrology, and chemistry of a Luna 16 basaltic fragment, sample B-1", "author": [ { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Chodos", "given_name": "A. A.", "clpid": "Chodos-A-A" }, { "family_name": "Gancarz", "given_name": "A. J.", "clpid": "Gancarz-A-J" }, { "family_name": "Haines", "given_name": "E. L.", "clpid": "Haines-E-L" }, { "family_name": "Papanastassiou", "given_name": "D. A.", "clpid": "Papanastassiou-D-A" }, { "family_name": "Ray", "given_name": "L.", "clpid": "Ray-L" }, { "family_name": "Tera", "given_name": "F.", "clpid": "Tera-F" }, { "family_name": "Wasserburg", "given_name": "G. J.", "orcid": "0000-0002-7957-8029", "clpid": "Wasserburg-G-J" }, { "family_name": "Wen", "given_name": "T.", "clpid": "Wen-T" } ], "abstract": "Luna 16 sample B-1 was the largest fragment (62 mg) obtained in the sample exchange with the USSR. Petrologic, mineralogic, and chemical investigations have been made on this fragment in conjunction with Rb-Sr and ^(40)Ar/^(39)Ar investigations by our colleagues. Sample B-1 is a fine-grained ophitic basalt but is distinguished from the Apollo samples by containing a single pyroxene, predominantly pigeonitic, an ilmenite content (7%) intermediate to that of the Apollo 11 and 12 samples, and subequal amounts of pyroxene (50%) and plagioclase (40%). Chemically it is distinguished by a high Sr content (437 ppm) and a high K/U value (4700). The K-content (1396 ppm) is higher than that of Luna 16 soil sample A-2.", "doi": "10.1016/0012-821X(72)90110-0", "issn": "0012-821X", "publisher": "Elsevier", "publication": "Earth and Planetary Science Letters", "publication_date": "1972-01", "series_number": "2", "volume": "13", "issue": "2", "pages": "353-367" }, { "id": "authors:5d23v-h0257", "collection": "authors", "collection_id": "5d23v-h0257", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221121-962044600.1", "type": "article", "title": "Uranium-bearing minerals of lunar rock 12013", "author": [ { "family_name": "Haines", "given_name": "E. L.", "clpid": "Haines-Eldon-L" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Chodos", "given_name": "A. A.", "clpid": "Chodos-A-A" }, { "family_name": "Wasserburg", "given_name": "G. J.", "orcid": "0000-0002-7957-8029", "clpid": "Wasserburg-G-J" } ], "abstract": "The U distribution in rock 12013 was studied by fission track and elemental mapping techniques. Major U-bearing phases are whitlockite, apatite, zircon, and phase \u03b2, which is a Zr-Ti mineral rich in Fe, Nb, Y, REE and containing up to 3.6% UO\u2082, 4.7% ThO\u2082, and 4.2% PbO. Calculated microprobe ages for phase \u03b2 average 4.0 AE and are in reasonable agreement with Rb-Sr and K-Ar ages. Phase \u03b2 plays a significant role in the U-Th-Pb systematics of rock 12013 and may play a similar role in the model ages of lunar soil.", "doi": "10.1016/0012-821x(71)90070-7", "issn": "0012-821X", "publisher": "Elsevier", "publication": "Earth and Planetary Science Letters", "publication_date": "1971-10", "series_number": "2", "volume": "12", "issue": "2", "pages": "145-154" }, { "id": "authors:wrwhf-x2e12", "collection": "authors", "collection_id": "wrwhf-x2e12", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180228-104559203", "type": "article", "title": "Petrologic and mineralogic investigation of some crystalline rocks returned by the Apollo 14 mission", "author": [ { "family_name": "Gancarz", "given_name": "A. J.", "clpid": "Gancarz-A-J" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Chodos", "given_name": "A. A.", "clpid": "Chodos-A-A" } ], "abstract": "Apollo 14 crystalline rocks (14053 and 14310) and crystalline rock fragments (14001,7,1; 14001,7,3; 14073; 14167,8,1 and 14321,191,X-1) on which Rb/Sr, ^(40)Ar-^(39)Ar, or cosmic ray exposure ages have been determined by our colleagues were studied with the electron microprobe and the petrographic microscope. Rock samples 14053 and 14310 are mineralogically and petrologically distinct from each other. On the basis of mineralogic and petrologic characteristics all of the fragments, except 14001,7,1, are correlative with rock 14310. Sample 14073 is an orthopyroxene basalt with chemical and mineralogic affinities to 'KREEP', the 'magic' and 'cryptic' components. Fragment 14001,7,1 is very similar to Luny Rock I.", "doi": "10.1016/0012-821X(71)90050-1", "issn": "0012-821X", "publisher": "Elsevier", "publication": "Earth and Planetary Science Letters", "publication_date": "1971-09", "series_number": "1", "volume": "12", "issue": "1", "pages": "1-18" }, { "id": "authors:ndbh6-7sj74", "collection": "authors", "collection_id": "ndbh6-7sj74", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151106-125849932", "type": "article", "title": "Mineralogy, Petrology, and Geochemistry of the Lunar Samples", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "On July 24, 1969, the first extraterrestrial samples, with the exception of meteorites, were returned to earth by Apollo 11. Since then these samples and the samples returned by Apollo 12 have been subjected to scientific investigations by hundreds of scientists from many countries. Drawing on advances from the last 25 years of study of meteorites and terrestrial rocks the variety and sophistication of the techniques used on these samples is truly impressive. It can truthfully be said that 10 years ago we could not have made the measurements, and that, even if we had had the data, we could not have interpreted it. The electron microprobe, the scanning electron microscope, and the mass spectrometer, as well as other instruments and techniques, have joined the microscope as routine tools with which to attack a petrologic problem.", "doi": "10.1029/EO052i005pIU090", "issn": "0096-3941", "publisher": "American Geophysical Union", "publication": "Eos", "publication_date": "1971-05", "series_number": "5", "volume": "52", "issue": "5", "pages": "90-100" }, { "id": "authors:v37c1-0p109", "collection": "authors", "collection_id": "v37c1-0p109", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220621-862339900", "type": "article", "title": "Mineralogic and isotopic investigations on lunar rock 12013", "author": [ { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Burnett", "given_name": "D. S.", "orcid": "0000-0001-9521-8675", "clpid": "Burnett-D-S" }, { "family_name": "Chodos", "given_name": "A. A.", "clpid": "Chodos-A-A" }, { "family_name": "Haines", "given_name": "Eldon L.", "clpid": "Haines-Eldon-L" }, { "family_name": "Huneke", "given_name": "J. C.", "clpid": "Huneke-J-C" }, { "family_name": "Papanastassiou", "given_name": "D. A.", "clpid": "Papanastassiou-D-A" }, { "family_name": "Podosek", "given_name": "F. A.", "clpid": "Podosek-F-A" }, { "family_name": "Russ", "given_name": "G. Price, III", "clpid": "Russ-G-Price-III" }, { "family_name": "Wasserburg", "given_name": "G. J.", "orcid": "0000-0002-7957-8029", "clpid": "Wasserburg-G-J" } ], "abstract": "Sample 12013, 10 was a sawn slab, 50 X 22 X 4 mm,\ncut from a position about 6 mm from an exterior surface\nof lunar sample 12013 returned from the Apollo\n12 mission. Because of its extreme heterogeneity it was\ndelivered to our clean-lab for division and distribution\nto the various principal investigators. Prior to division\nit was carefully examined and photographed and preliminary\nRb/Sr and microprobe results were obtained\non loose fragments found in the sample container.\nThin section 12013, 4 (Apollo 12 sample catalog)\nfrom an unknown part of the sample also provided\nsome guidance in the distribution.", "doi": "10.1016/0012-821x(70)90046-4", "issn": "0012-821X", "publisher": "Elsevier", "publication": "Earth and Planetary Science Letters", "publication_date": "1970-09-01", "series_number": "2", "volume": "9", "issue": "2", "pages": "137-163" }, { "id": "authors:f71hs-wyj76", "collection": "authors", "collection_id": "f71hs-wyj76", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130220-113109469", "type": "article", "title": "Ages, Irradiation History, and Chemical Composition of Lunar Rocks from the Sea of Tranquillity", "author": [ { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Burnett", "given_name": "D. S.", "orcid": "0000-0001-9521-8675", "clpid": "Burnett-D-S" }, { "family_name": "Chodos", "given_name": "A. A.", "clpid": "Chodos-A-A" }, { "family_name": "Eugster", "given_name": "O. J.", "clpid": "Eugster-O-J" }, { "family_name": "Huneke", "given_name": "J. C.", "clpid": "Huneke-J-C" }, { "family_name": "Papanastassiou", "given_name": "D. A.", "clpid": "Papanastassiou-D-A" }, { "family_name": "Podosek", "given_name": "F. A.", "clpid": "Podosek-F-A" }, { "family_name": "Russ", "given_name": "G. Price, II", "clpid": "Russ-G-P-II" }, { "family_name": "Sanz", "given_name": "H. G.", "clpid": "Sanz-H-G" }, { "family_name": "Tera", "given_name": "F.", "clpid": "Tera-F" }, { "family_name": "Wasserburg", "given_name": "G. J.", "orcid": "0000-0002-7957-8029", "clpid": "Wasserburg-G-J" } ], "abstract": "The ^(87)Rb-^(87)Sr internal isochrons for five rocks yield an age of 3.65\u00b10.05 \u00d7 10^9 years which presumably dates the formation of the Sea of Tranquillity. Potassium-argon ages are consistent with this result. The soil has a model age of 4.5 \u00d7 10^9 years, which is best regarded as the time of initial differentiation of the lunar crust. A peculiar rock fragment from the soil gave a model age of 4.44 \u00d7 10^9 years. Relative abundances of alkalis do not suggest differential volatilization. The irradiation history of lunar rocks is inferred from isotopic measurements of gadolinium, vanadium, and cosmogenic rare gases. Spallation xenon spectra exhibit a high and variable 1^(31)Xe/^(126)Xe ratio. No evidence for ^(129)I was found. The isotopic composition of solar-wind xenon is distinct from that of the atmosphere and of the average for carbonaceous chondrites, but the krypton composition appears similar to average carbonaceous chondrite krypton.", "doi": "10.1126/science.167.3918.463", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1970-01-30", "series_number": "3918", "volume": "167", "issue": "3918", "pages": "463-466" }, { "id": "authors:r02q8-s1w85", "collection": "authors", "collection_id": "r02q8-s1w85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220909-223202700", "type": "article", "title": "A petrogenetic grid for the Fe-Mg silicates of pelitic schists", "author": [ { "family_name": "Albee", "given_name": "Arden L.", "clpid": "Albee-A-L" } ], "abstract": "The topology of the reaction surfaces for the phases-garnet, chloritoid, staurolite, kyanite, cordierite, chlorite, and biotite-is shown for two limiting sections of P\u209b, T, PH\u2082O space for the part of the system-SiO\u2082-Al\u2082O\u2083-FeO-MgO-K\u2082O-H\u2082O in which quartz and muscovite are stable. The basic assumption made is that the course of progressive metamorphism is primarily one of progressive dehydration with a progressive restriction of the fields of the most hydrous minerals, notably chlorite. The resulting petrogenetic grids for the surfaces P\u209b \u2248 PH\u2082O and Ps \u2248 \u03c1s/\u03c1H\u2082O are predominantly theoretical and should serve as a useful check in assigning natural metamorphic sequences to their relative pressure-temperature relationships.", "doi": "10.2475/ajs.263.6.512", "issn": "0002-9599", "publisher": "American Journal of Science", "publication": "American Journal of Science", "publication_date": "1965-06-01", "series_number": "6", "volume": "263", "issue": "6", "pages": "512-536" }, { "id": "authors:qc158-qvr29", "collection": "authors", "collection_id": "qc158-qvr29", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141110-110243393", "type": "article", "title": "Migration of radiogenic strontium during metamorphism", "author": [ { "family_name": "Wasserburg", "given_name": "G. J.", "orcid": "0000-0002-7957-8029", "clpid": "Wasserburg-G-J" }, { "family_name": "Albee", "given_name": "A. L.", "clpid": "Albee-A-L" }, { "family_name": "Lanphere", "given_name": "M. A.", "clpid": "Lanphere-M-A" } ], "abstract": "Study of the concentration and isotopic composition of strontium and rubidium in hornblende diorite dikes and sills of Precambrian age from the Panamint Mountains of California showed that these rock systems were enriched in radiogenic Sr during a late Mesozoic metamorphism. Enrichments in radiogenic Sr were observed for total-rock samples which yielded apparent ages of up to 34,000 m.y., although there is no obvious petrographic evidence for such metasomatic changes. These results indicate that some caution is necessary in interpreting the Sr isotopic composition of rocks in terms of their original source or in assuming that 'total rocks' form closed systems. In general, the initial isotopic Sr composition should be determined, not assumed.", "doi": "10.1029/JZ069i020p04395", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research", "publication_date": "1964-10-15", "series_number": "20", "volume": "69", "issue": "20", "pages": "4395-4401" } ]