@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/102990,
    title ="The Unearthly Landscapes of Mars",
    author = "Albee, Arden L.",
    journal = "Scientific American",
    volume = "288",
    number = "6",
    pages = "44-53",
    month = "June",
    year = "2003",
    doi = "10.1038/scientificamerican0603-44",
    issn = "0036-8733",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20200505-072751563",
    note = "© 2003 Scientific American.",
    revision_no = "5",
    abstract = "The Red Planet is no dead planet.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39729,
    title ="Martian rocks, minerals, and mantles",
    author = "Albee, Arden",
    journal = "Meteoritics and Planetary Science",
    volume = "37",
    number = "S5",
    pages = "A9-A9",
    month = "May",
    year = "2002",
    doi = "10.1111/j.1945-5100.2002.tb00912.x",
    issn = "1086-9379",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130802-104030044",
    note = "© 2002 Meteoritical Society.\nArticle first published online: 26 Jan. 2010.",
    revision_no = "9",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39730,
    title ="Introduction to the special section: The Mars Global Surveyor mission",
    author = "Albee, Arden",
    journal = "Journal of Geophysical Research E",
    volume = "106",
    number = "E10",
    pages = "23289-23289",
    month = "October",
    year = "2001",
    doi = "10.1029/2001JE001511",
    issn = "0148-0227",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130802-104725010",
    note = "© 2001 by the American Geophysical Union.\n\nReceived May 1, 2001; revised May 9, 2001;\naccepted June 6, 2001.\n\n",
    revision_no = "9",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/45890,
    title ="Overview of the Mars Global Surveyor mission",
    author = "Albee, Arden L. and Arvidson, Raymond E.",
    journal = "Journal of Geophysical Research E",
    volume = "106",
    number = "E10",
    pages = "23291-23316",
    month = "October",
    year = "2001",
    doi = "10.1029/2000JE001306",
    issn = "0148-0227",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20140522-104604508",
    note = "© 2001 American Geophysical Union. Received June 30, 2000; revised February 9, 2001; accepted February 12, 2001. \n\nThe research was carried out by the Mars Global Surveyor Project at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics\nand Space Administration. A. A. was Project Scientist, F.P. was Deputy Project Scientist, and T.T. was Science Manager and subsequently Mission Manager and Project Manager of the Project. R.E.A. was supported as a Mars Surveyor Program\nInterdisciplinary Scientist by JPL contract 1204044 to Washington University. The authors acknowledge the contribution of the entire project staff, including their colleagues at Lockheed Martin Aerospace and at all the home institutions of the instrument Principal Investigators and the Radio Science Team Leader. Many of the key project members and scientists were part of the early studies in 1981-1982 that led to Mars Observer and then to Mars Global Surveyor. Glenn Cunningham was project manager during the period from when Mars Observer was lost until the beginning\nof the mappingp eriod. His contribution to the amazing\nsuccess of MGS was outstanding; upon three occasions he made difficult decisions that preserved the scientific integrity of the mission. As spacecraft system manager throughout Mars Observer and MGS development, George Pace was always watchful for \"creeping science requirements\", but his selection of a larger HGA nearly doubled the\ncapability for science downlink. Much of this work was drawn from a variety of project documents and we thank their authors, particularly Glenn Cunningham, Pat Esposito, Wayne Lee, and George Pace. Pat Esposito carefully checked\nthe sections on mission and mission operations. We thank Pat Esposito, Wayne Lee, Mike Malin, Tim Parker, and Susan Slavney for help in figure and table generation.",
    revision_no = "11",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/634,
    title ="Mars 2000",
    author = "Albee, Arden L.",
    journal = "Annual Review of Earth and Planetary Sciences",
    volume = "28",
    
    pages = "281-304",
    month = "May",
    year = "2000",
    doi = "10.1146/annurev.earth.28.1.281",
    issn = "0084-6597",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:ALBareps00",
    note = "© 2000 by Annual Reviews. \n\nWorking with all the scientists and engineers associated with the Mars Observer and Mars Global Surveyor projects over the last 20 years has been a rewarding and unbelievable learning experience. More than 400 attendees at the Fifth International Conference on Mars in July 1999 helped to shape this summary, but I particularly want to thank the invited speakers who presented specialized reviews and prepared extended abstracts (CD-ROM Contribution, 972. The Lunar & Planetary Institute. Houston, Texas). In many instances where I used these abstracts, I have actually cited recent or ‘‘In press’’ papers to acknowledge the contribution.",
    revision_no = "9",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39731,
    title ="Mars Global Surveyor Mission: Overview and Status",
    author = "Albee, A. L. and Palluconi, F. D.",
    journal = "Science",
    volume = "279",
    number = "5357 ",
    pages = "1671-1672",
    month = "March",
    year = "1998",
    doi = "10.1126/science.279.5357.1671",
    issn = "0036-8075",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130802-105543692",
    note = "© 1998 American Association for the Advancement of Science. Received 21 January 1998; accepted 18 February 1998.\n\nThe authors are the Project Scientist (A.L.A.), Deputy\nProject Scientist (F.D.P.), and the Interdisciplinary\nScientist responsible for Data Archiving\n(R.E.A.) for the Mars Global Surveyor Mission. We\nare indebted to engineers at the Jet Propulsion\nLaboratory and LMA who have devoted themselves\nto this mission over the years and who operate\nthe spacecraft today. Our special acknowledgement\ngoes to Glen Cunningham, Project Manager.\nPortions of the work described in this paper\nwere performed by the Jet Propulsion Laboratory\nunder contract to the National Aeronautics and\nSpace Administration.",
    revision_no = "10",
    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. ",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39738,
    title ="Mars Global Surveyor: Ready for launch in November 1996",
    author = "Palluconi, Frank D. and Albee, Arden L.",
    journal = "Acta Astronautica",
    volume = "40",
    number = "2-8",
    pages = "511-516",
    month = "January",
    year = "1997",
    doi = "10.1016/S0094-5765(97)00115-X",
    issn = "0094-5765",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130802-134910991",
    note = "© 1997 International Astronautical Federation. Published by Elsevier Science Ltd.\n\nThe work described in this paper was performed by the\nJet Propulsion Laboratory, California Institute of\nTechnology under contract to the National Aeronautics\nand Space Administration. The authors wish to\nacknowledge the work of the many members of the\nMGS project team who conducted the work on which\nthis report is based.",
    revision_no = "12",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/50905,
    title ="Mission to Mars to Collect a Storehouse of Scientific Data",
    author = "Albee, Arden",
    journal = "Eos",
    volume = "77",
    number = "45",
    pages = "441-442",
    month = "November",
    year = "1996",
    doi = "10.1029/96EO00295",
    issn = "0096-3941",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20141028-083851671",
    note = "© 1996 American Geophysical Union.",
    revision_no = "10",
    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—most of\nall—comparative planetology.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39740,
    title ="Foreword [to special section on Mars Observer]",
    author = "Albee, Arden",
    journal = "Journal of Geophysical Research E",
    volume = "97",
    number = "E5",
    pages = "7663-7663",
    month = "May",
    year = "1992",
    doi = "10.1029/92JE00724",
    issn = "0148-0227",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130802-140812019",
    note = "© 1992 by the American Geophysical Union.\n\n",
    revision_no = "10",
    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.\n",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39768,
    title ="Mars Observer mission",
    author = "Albee, A. L. and Arvidson, R. E.",
    journal = "Journal of Geophysical Research E",
    volume = "97",
    number = "E5",
    pages = "7665-7680",
    month = "May",
    year = "1992",
    doi = "10.1029/92JE00342",
    issn = "0148-0227",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130805-142011822",
    note = "© 1992 by the American Geophysical Union.\n\nReceived May 6, 1991; \nrevised February 11, 1992;\naccepted February 12, 1992.\n\nThe research described here was carried out\nby the Mars Observer Project at the Jet Propulsion Laboratory,\nCalifornia Institute of Technology, under contract with the National\nAeronautics and Space Administration. R.E.A. was supported by\nJPL contract 957584 to Washington University. The authors acknowledge\nthe contribution of the entire project staff. The science\nobjectives for the individual investigations are summarized from the\nscience plans prepared by the lead investigators.",
    revision_no = "10",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/44925,
    title ="Mars Observer: The Next Mars Mission",
    author = "Albee, Arden L. and Palluconi, Frank D.",
    journal = "Journal of Spacecraft and Rockets",
    volume = "28",
    number = "5",
    pages = "498-500",
    month = "September",
    year = "1991",
    doi = "10.2514/3.26272",
    issn = "0022-4650",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20140414-113245594",
    note = "© 1991 American Institute of Aeronautics and Astronautics, Inc. Received Dec. 11, 1989; revision received Oct. 2, 1990; accepted for publication March 30, 1991. The U.S. Government\nhas a royalty-free license to exercise all rights under the copyright claimed herein for Governmental purposes. All other rights are reserved by the copyright owner. This research was conducted at the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, under contract with NASA. The authors wish to thank members of the Mars Observer Project Science Group for providing experiment descriptions used in the preparation of this paper.",
    revision_no = "11",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/42009,
    title ="Advances in the development of encapsulants for mercuric iodide X-ray detectors",
    author = "Iwanczyk, J. S. and Wang, Y. J.",
    journal = "IEEE Transactions on Nuclear Science",
    volume = "37",
    number = "6",
    pages = "2214-2218",
    month = "December",
    year = "1990",
    doi = "10.1109/23.101259   ",
    issn = "0018-9499",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20131022-112714082",
    note = "© 1990 IEEE. Manuscript received January 17, 1990; revised June 26, 1990. This work was sponsored by the National Aeronautics and Space Administration and supported in part by NIH grant #5R01 GM 37161.\nThe valuable technical assistance of Mrs. F. Riquelme, Messrs. N. Dorri and B. Dancy of USC, and Mr. V. Taylor at JPL are greatly appreciated.",
    revision_no = "9",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/51644,
    title ="Mars Observer's Global Mapping Mission",
    author = "Albee, A. L. and Palluconi, D. F.",
    journal = "Eos",
    volume = "71",
    number = "39",
    pages = "1099-1107",
    month = "September",
    year = "1990",
    doi = "10.1029/EO071i039p01099-01",
    issn = "0096-3941",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20141112-102957806",
    note = "© 1990 American Geophysical Union.\n\nThe research described here was carried\nout by the Mars Observer Project at the Jet\nPropulsion Laboratory, California Institute of\nTechnology, under contract with the National\nAeronautics and Space Administration. The\nauthors are the project scientists for the Mars\nObserver mission and acknowledge the contribution\nof the entire project staff. The science\nobjectives for the individual investigations\nare summarized from the science plans\nprepared by the individual investigators.",
    revision_no = "8",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39817,
    title ="Practical Application of HgI_2 Detectors to a Space-Flight Scanning Electron-Microscope",
    author = "Bradley, J. G. and Conley, J. M.",
    journal = "Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment",
    volume = "283",
    number = "2",
    pages = "348-351",
    month = "November",
    year = "1989",
    doi = "10.1016/0168-9002(89)91383-1",
    issn = "0168-9002",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130808-104603861",
    note = "©1989 Elsevier Science Publishers B.V.\n\nReceived 26 May 1989.\n\nThe contributions to this work by V. Taylor, B.\nDancy and F. Riquelme are greatly appreciated.\nThe research described in this paper was performed,\nin part, by the Jet Propulsion Laboratory, California\nInstitute of Technology and the University of Southern\nCalifornia, and was jointly sponsored by the National\nAeronautics and Space Administration and Caltech\nthrough the Caltech President's Fund.",
    revision_no = "12",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/42005,
    title ="Performance and durability of HgI_2 X-ray detectors for space missions",
    author = "Iwanczyk, J. S. and Wang, Y. J.",
    journal = "IEEE Transactions on Nuclear Science",
    volume = "36",
    number = "1",
    pages = "841-845",
    month = "February",
    year = "1989",
    doi = "10.1109/23.34562   ",
    issn = "0018-9499",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20131022-110416691",
    note = "© 1989 IEEE.\nThe research described in this paper was sponsored\nby the National Aeronautics and Space Administration.\nThe work performed at the University of Southern\nCalifornia Institute of Physics was also supported by\nNIH grant #5R01 GM37161. The valuable technical\nassistance of Mrs. F. Riquelme and Messrs N. Dorri and\nB. Dancy of USC and Mr. V. Taylor of JPL is greatly\nappreciated. The text was edited by Ms. S.L. Segall.\n",
    revision_no = "10",
    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_α 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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/52949,
    title ="The Analysis of Extraterrestrial Materials [Book Review]",
    author = "Albee, Arden L.",
    journal = "Eos",
    volume = "69",
    number = "25",
    pages = "670",
    month = "June",
    year = "1988",
    doi = "10.1029/88EO00227",
    issn = "0096-3941",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20141217-100113797",
    note = "© 1988 American Geophysical Union.\n\nBook review of: Isidore Adler, Chem. Anal. Ser., vol. 8, John\nWiley, New York, xvii + 346 pp., 1986.",
    revision_no = "8",
    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 — 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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39769,
    title ="Scanning Electron-Microscopes and Other Beam Instruments for Spaceflight",
    author = "Albee, Arden L.",
    journal = "Journal of Electron Microscopy Technique",
    volume = "7",
    number = "2",
    pages = "137-137",
    month = "October",
    year = "1987",
    
    issn = "0741-0581",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130805-150254709",
    note = "© 1987 Wiley-Liss, Inc.\n\nArticle first published online: 4 Feb. 2005.",
    revision_no = "13",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/41749,
    title ="Low Energy X-Ray Spectra Measured with a Mercuric Iodide Energy Dispersive Spectrometer in a Scanning Electron Microscope",
    author = "Iwanczyk, J. S. and Dabrowski, A. J.",
    journal = "IEEE Transactions on Nuclear Science",
    volume = "33",
    number = "1",
    pages = "355-358",
    month = "February",
    year = "1986",
    doi = "10.1109/TNS.1986.4337118",
    issn = "0018-9499",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20131008-143821891",
    note = "© 1986 IEEE.\nPublished: Feb. 1986.\nThe authors wish to thank B. Dancy, F. Riquelme\nand P. Rohmer at USC and V. Taylor at JPL for valuable\ntechnical assistance. Research described in this paper\nwas performed, in part, by Jet Propulsion Laboratory,\nCalifornia Institute of Technology under NASA Contract\nNAS 7-918. Fundamental HgI2 x-ray detector development\nat USC was supported by DOE Contract DE-AM03-76SF00113\nand NASA Contract NSG-7535.\n\n",
    revision_no = "14",
    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-Kα\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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/54697,
    title ="Kimberlites I: Kimberlites and Related Rocks. Kimberlites II: The Mantle and Crust-Mantle Relationships [Book Review]",
    author = "Albee, Arden L.",
    journal = "Eos",
    volume = "66",
    number = "7",
    pages = "63",
    month = "February",
    year = "1985",
    doi = "10.1029/EO066i007p00063",
    issn = "0096-3941",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20150211-091223549",
    note = "© 1985 American Geophysical Union.",
    revision_no = "9",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/44919,
    title ="Distribution of Ordovician and Devonian metamorphism in mafic and pelitic schists from northern Vermont",
    author = "Laird, Jo and Lanphere, Marvin A.",
    journal = "American Journal of Science",
    volume = "284",
    number = "4-5",
    pages = "376-413",
    month = "May",
    year = "1984",
    doi = "10.2475/ajs.284.4-5.376",
    issn = "0002-9599",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20140414-105654946",
    note = "© 1984 American Journal of Science. American Journal of Science Online May 1984. We thank Henry Shaw for doing the electron microprobe analyses of the additional samples of mafic schist and James R. Anderson for helping make the amphibole separates. G. P. Kraker, D. H. Rusling, and the\noperational staff of the U.S. Geological Survey reactor facility managed the fast neutrons required for this study. S. E. Kollman, J. Y. Saburomaru, and J. C. Von Essen assisted with the argon measurements. Theoretical concepts developed by J. B. Thompson, Jr. have been invaluable to our\npetrologic studies. Discussions with countless New England geologists have helped put the data into geological perspective. Reviews by E. A. Downie, C. V. Guidotti, and J. F. Sutter are sincerely appreciated. We gratefully acknowledge financial support from the National Science Foundation (#DES 69-0064 and EAR 75-03416 to A.L.A.).",
    revision_no = "8",
    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. ",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/52768,
    title ="Scanning Electron Microscopy and X-Ray Microanalysis [Book Review]",
    author = "Albee, Arden L.",
    journal = "Eos",
    volume = "63",
    number = "47",
    pages = "1188",
    month = "November",
    year = "1982",
    doi = "10.1029/EO063i047p01188",
    issn = "0096-3941",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20141212-131937251",
    note = "© 1982 American Geophysical Union.\n\nBook review of: Scanning Electron Microscopy and X-Ray\nMicroanalysis by J. I. Goldstein, D. E. Newbury, P. Echlin,\nD. C. Joy, C. Fiori, and E. Lifshin, Plenum,\nNew York, xii + 673 pp., 1981.",
    revision_no = "8",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/44924,
    title ="Crystallization Paths of Leucite-Bearing Lavas: Examples from Italy",
    author = "Baldridge, W. Scott and Carmichael, I. S. E.",
    journal = "Contributions to Mineralogy and Petrology",
    volume = "76",
    number = "3",
    pages = "321-335",
    month = "May",
    year = "1981",
    doi = "10.1007/BF00375459",
    issn = "0010-7999",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20140414-111513915",
    note = "© 1981 Springer-Verlag. Received July 26, 1980; Accepted February 6, 1981. We are grateful to A. Chodos and R. Hagan for their expert assistance in the electron microprobe laboratories at Caltech and Los Alamos National Laboratory, respectively. W.G. Melson of the Smithsonian Institution kindly provided us with Washington's original samples. Work carried out at Caltech was supported by National Science Foundation grant GA-12867 and that at Berkeley by NSF grant DES 74-12782. This work was completed at the Los Alamos \nNational Laboratory under the support of the Office of Basic Energy Sciences of the U.S. Department of Energy.",
    revision_no = "11",
    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° C±100) 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 haüyne 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° C to 1,150° 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.\n",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/44911,
    title ="High-pressure metamorphism in mafic schist from northern Vermont",
    author = "Laird, Jo and Albee, Arden L.",
    journal = "American Journal of Science",
    volume = "281",
    number = "2",
    pages = "97-126",
    month = "February",
    year = "1981",
    doi = "10.2475/ajs.281.2.97 ",
    issn = "0002-9599",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20140414-093459837",
    note = "© 1981 American Journal of Science.\nContribution 3042, Publications of the Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125. We thank A. H. Chidester for providing several samples, including one of those studied in detail (A-Bl-100), and W. M. Cady for sending copies of field notes, field maps, and thin section descriptions made by Cady, Albee, and Chidester in their study of Tillotson Peak. Data collection for this project was aided by the fact that A. A. Chodos keeps the\nCaltech electron microprobe in top running condition. This paper has certainly benefitted from the reviews of P. Robinson, A. B. Thompson, and W. E. Trzcienski, Jr. We gratefully acknowledge financial support from National Science Foundation Grants DES 69-0064 and EAR 75-03416 to A.L.A. and Geological Society of America Penrose Bequest Research Grants 1554-71 and 1670-72 to J.L. The senior author also wishes to thank the Institut für Kristallographie und Petrographie, Eidgenossische Technische Hochschule Zürich, for support during the writing of later drafts of this manuscript.\n",
    revision_no = "11",
    abstract = "The only confirmed occurrence of glaucophane and omphacite in the Appalachian Mountains of New England is in mafic schist from Tillotson Peak (44°48', 72°33'), north-central Vermont. Mineral assemblages observed, all with epidote\n+ sphene ± magnetite ± phengitic muscovite ± carbonate (calcite or dolomite) ± apatite ± 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): □ (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•) 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 ± 2 kb and 450 ± 100°C with P_(h2O) ≈ P_(Total). It is proposed that the metamorphism occurred during the Ordovician.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/44915,
    title ="Pressure, temperature, and time indicators in mafic schist; their application to reconstructing the polymetamorphic history of Vermont",
    author = "Laird, Jo and Albee, Arden L.",
    journal = "American Journal of Science",
    volume = "281",
    number = "2",
    pages = "127-175",
    month = "February",
    year = "1981",
    doi = "10.2475/ajs.281.2.127 ",
    issn = "0002-9599",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20140414-102536185",
    note = "© 1981 American Journal of Science. Contribution No. 3043, Publications of the Division of Geological and Planetary\nSciences, California Institute of Technology, Pasadena, California 91125. We thank the many geologists whose geologic maps helped direct the sampling for this project. Discussions in and out of the field with J. R. Anderson, J. L. Rosenfeld, and J. B. Thompson, Jr. were especially\nbeneficial. Marrion Hood, Evelyn and Morgan Potter, and Elizabeth Wheelwright extended true Yankee hospitality during the field seasons. The collection of mineral compositional data was aided enormously by the expertise of A. A. Chodos in the operation and maintenance of the\nCaltech electron microprobe. Constructive criticism by the reviewers of this paper, P. Robinson, R. J. Tracy, and A. B. Thompson, are appreciated. Support from National Science Foundation Grants DES 69-0064 and EAR 75-03416 to A.L.A. and Geological Society of America Penrose Bequest Research Grants 1554-71 and 1670-72 to J.L. are gratefully acknowledged. The senior author wishes to thank the Institut für Kristallographie und Petrographie,  Eidgenossische Technische Hochschule Zürich for financial support during the writing of later drafts of this manuscript.",
    revision_no = "12",
    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 ± carbonate ± K-mica ± 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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/41926,
    title ="Stratigraphy, structure, and metamorphism in the central Panamint Mountains (Telescope Peak quadrangle), Death Valley area, California: Summary",
    author = "Labotka, Theodore C. and Albee, Arden L.",
    journal = "Geological Society of America Bulletin",
    volume = "91",
    number = "3",
    pages = "125-129",
    month = "March",
    year = "1980",
    doi = "10.1130/0016-7606(1980)91<125:SSAMIT>2.0.CO;2 ",
    issn = "0016-7606",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20131015-145647213",
    note = "© 1980 Geological Society of America.\n\nManuscript received by the Society March 19, 1979; Revised manuscript received October 8, 1979; Manuscript accepted October 24, 1979.\n\nField work in the Panamint Mountains was supported by grants\nfrom the National Science Foundation to Albee and from the\nGeological Society of America to Lanphere, McDowell, and\nLabotka. The staff members of Death Valley National Monument\nhave been of great assistance during the course of the field work.\nWe have benefited from stimulating discussions about Death Valley\ngeology, many of them in the field, with R. H. Jahns, R. E. Powell,\nL. T. Silver, J. H. Stewart, G. R. Tilton, B. W. Troxel, G. J. Wasserburg,\nand L. A. Wright. Critical reviews by B. C. Burchfiel and\nB. W. Troxel have improved the readability of the manuscript.",
    revision_no = "11",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/41928,
    title ="Silica solid solution and zoning in natural plagioclase",
    author = "Beaty, David W. and Albee, Arden",
    journal = "American Mineralogist",
    volume = "65",
    number = "1-2",
    pages = "63-74",
    month = "January",
    year = "1980",
    
    issn = "0003-004X",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20131015-154255329",
    note = "© 1980 Mineralogical Society of America.\nManuscript received, May 21, 1979;\naccepted for publication, October l, 1979.\nDiscussions with John Longhi, Bob Dymek, and George Rossman\nstimulated the authors' interest in this study. The data were\ncollected by several Caltech graduate students between 1975 and\n1978 as parts of their theses and research projects. Bob Gregory\nand Scott Baldridge were particularly generous with their unpublished\ndata. The manuscript was typed by Lou Ann Cordell and\nBetty Robinson. Early comments by Bob Gregory and George\nRossman and thorough reviews by Tim Grove and John Longhi\nhave significantly improved the manuscript. The support of\nNASA grant NGL-05-002-338 is gratefully acknowledged.\n",
    revision_no = "9",
    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.\n",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/42529,
    title ="Serpentinization of the Belvidere Mountain ultramafic body, Vermont; mass balance and reaction at the metasomatic front",
    author = "Labotka, Theodore C. and Albee, Arden L.",
    journal = "Canadian Mineralogist",
    volume = "17",
    number = "4",
    pages = "831-845",
    month = "November",
    year = "1979",
    
    issn = "0008-4476",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20131118-132153939",
    note = "© 1979 Mineralogical Association of Canada. Received October 1978, revised manuscript accepted\nJuly 1979. The perceptive review by F.J. Wicks is greatly appreciated. Support was provided by National Science Foundation grant EAR 75-03416.",
    revision_no = "12",
    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. ",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39794,
    title ="Titanium and Aluminum in Biotite From High-Grade Archaean Gneisses, Langø, West Greenland",
    author = "Dymek, R. F. and Albee, A. L.",
    journal = "Transactions - American Geophysical Union",
    volume = "58",
    number = "6",
    pages = "525-525",
    month = "June",
    year = "1977",
    
    issn = "0002-8606",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130806-152922789",
    note = "© 1977 American Geophysical Union.\n",
    revision_no = "15",
    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.\n",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/41999,
    title ="Petrography of isotopically-dated clasts in the Kapoeta howardite and petrologic constraints on the evolution of its parent body",
    author = "Dymek, R. F. and Albee, A. L.",
    journal = "Geochimica et Cosmochimica Acta",
    volume = "40",
    number = "9",
    pages = "1115-1130",
    month = "September",
    year = "1976",
    doi = "10.1016/0016-7037(76)90053-3",
    issn = "0016-7037",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20131021-154533262",
    note = "© 1976 Pergamon Press.\n\nReceived 5 August 1915; accepted in revised form 8 March 1976.\n\nWe wish to thank Dr. A. H. ISHAG and Dr. A. WIDATALLA, Geological Survey of the Sudan,\nfor their kind and generous cooperation in allowing us access to samples of Kapoeta. In addition, we wish to\nthank Dr. R. S. RAJAN for arranging the transfer of Basalt Clast ρ to this laboratory, and Dr. M. W. ROWE for providing\nus with this very important sample. We have benefited from discussions with M. DAILY, D. A. PAPANASTASSIOU,\nR. S. RAJAN, S. P. SMITH, and E. M. STOLPER. We would especially like to thank J. C. HUNEKE for extremely helpful\ndiscussions and encouragement throughout the course of this study. Our research on Kapoeta has been supported\nby NSF Grant GP-28027 and NASA Grant NGL-05-002-338. The microprobe laboratory has been developed\nwith the support of the National Science Foundation, the Jet Propulsion Laboratory, and the Union Pacific\nFoundation. This paper has benefited from thorough reviews by A. M. REID and J. L. WARNER, and comments\non the manuscript by R. BRETT and O. JAMES.\n",
    revision_no = "11",
    abstract = "Detailed mineralogic and petrographic data are presented for four isotopically-dated basaltic rock fragments separated from the howardite Kapoeta. Clasts C and ρ have been dated at ~4.55 AE and ~ 4.60 AE respectively, and Clast ρ 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 ⪆ 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—basaltic (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.\n",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/39777,
    title ="A review of lunar sample studies and their application to studies of the terrestrial planets",
    author = "Albee, Arden L.",
    journal = "Reviews of Geophysics and Space Physics",
    volume = "13",
    number = "3",
    pages = "419-422",
    month = "July",
    year = "1975",
    doi = "10.1029/RG013i003p00419",
    issn = "0034-6853",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130806-100459556",
    note = "© 1975 by the American Geophysical Union.\nContribution 2567 of the Division of Geological and Planetary Sciences, California Institute of Technology,\nPasadena, California.",
    revision_no = "8",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/85262,
    title ="Constrained least-squares analysis of petrologic problems with an application to lunar sample 12040",
    author = "Reid, M. J. and Gancarz, A. J.",
    journal = "Earth and Planetary Science Letters",
    volume = "17",
    number = "2",
    pages = "433-445",
    month = "January",
    year = "1973",
    doi = "10.1016/0012-821X(73)90212-4",
    issn = "0012-821X",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20180313-073633736",
    note = "© 1973 Published by Elsevier B.V. \n\nReceived 22 August 1972, Revised 25 October 1972. \n\nWe are grateful to D. Muhleman for a long series of discussions on various aspects of this paper and to D. Muhleman, S. Delong, and R. Dean for their comments on a preliminary draft of the paper. G.J. Wasserburg initiated the work on sample 12040 and pointed out that we do not really understand a rock unless we can explain the complete phase distribution of every element. The work was supported by NAS contract NAS-9-8074 and NSF grant GA-12867. The micro probe laboratory has been developed with the support of the Jet Propulsion Laboratory, National Science Foundation, and the Union Pacific Foundation. One of us (A.J.G.) holds a National Science Foundation Graduate Fellowship.",
    revision_no = "10",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/85166,
    title ="Comparative petrology of Apollo 16 sample 68415 and Apollo 14 samples 14276 and 14310",
    author = "Gancarz, A. J. and Albee, A. L.",
    journal = "Earth and Planetary Science Letters",
    volume = "16",
    number = "3",
    pages = "307-330",
    month = "November",
    year = "1972",
    doi = "10.1016/0012-821X(72)90150-1",
    issn = "0012-821X",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20180307-083914238",
    note = "© 1972 Published by Elsevier B.V. \n\nReceived 25 September 1972. \n\nWe have greatly benefited from a series of heated discussions with G.J. Wasserburg and D. Papanastassiou, and from detailed comments upon the manuscript by R. Dymek, C. Gray, J.C. Huneke, D. Papanastassiou, and G.J. Wasserburg. E. Haines provided fission-track data on sample 14276. This work was supported by NASA contract NAS-9-8074. The microprobe laboratory has been developed with the support of NSF, JPL, and the Union Pacific Foundation.",
    revision_no = "11",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/85009,
    title ="Mineralogy, petrology, and chemistry of a Luna 16 basaltic fragment, sample B-1",
    author = "Albee, A. L. and Chodos, A. A.",
    journal = "Earth and Planetary Science Letters",
    volume = "13",
    number = "2",
    pages = "353-367",
    month = "January",
    year = "1972",
    doi = "10.1016/0012-821X(72)90110-0",
    issn = "0012-821X",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20180228-105651836",
    note = "© 1972 Published by Elsevier B.V. \n\nReceived 16 November 1971, Revised 29 November 1971. \n\nWe are grateful to the Academy of Sciences of the USSR for making it possible for us to work on these samples. We greatly appreciate the confidence which The Lunar Sample Analysis Planning Team and the curator of the lunar samples have shown by entrusting us with the handling of such a extremely valuable sample. We are indebted to Jack Huneke for valid criticism of the manuscript and to Paul Cast for a useful discussion of the Sr/Eu relationships. Joe Brown meticulously prepared the micro-thin sections. \n\nThe work was supported by NASA contracts NAS 9-8074 and NA 7-100. The microprobe laboratory has been developed with the support of NSF, JPL, and the Union Pacific Foundation.",
    revision_no = "9",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/85007,
    title ="Petrologic and mineralogic investigation of some crystalline rocks returned by the Apollo 14 mission",
    author = "Gancarz, A. J. and Albee, A. L.",
    journal = "Earth and Planetary Science Letters",
    volume = "12",
    number = "1",
    pages = "1-18",
    month = "September",
    year = "1971",
    doi = "10.1016/0012-821X(71)90050-1",
    issn = "0012-821X",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20180228-104559203",
    note = "© 1971 Published by Elsevier B.V. \n\nReceived 4 August 1971, Revised 11 August 1971. \n\nWe gratefully acknowledge G.J. Wasserburg for his care and foresight in selecting fragments from the soft and breccia samples. Continuing discussions with G.J. Wasserburg and other Lunatics have proved invaluable. E.L. Haines provided the fission track data and Mr. Joe Brown meticulously prepared the micro-thin sections. This work was supported by NASA contract NAS-9-8074. The microprobe laboratory has been developed with the support of NSF, JPL and the Union Pacific Foundation.",
    revision_no = "8",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/61949,
    title ="Mineralogy, Petrology, and Geochemistry of the Lunar Samples",
    author = "Albee, Arden L.",
    journal = "Eos",
    volume = "52",
    number = "5",
    pages = "90-100",
    month = "May",
    year = "1971",
    doi = "10.1029/EO052i005pIU090",
    issn = "0096-3941",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20151106-125849932",
    note = "© 1971 American Geophysical Union.",
    revision_no = "7",
    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.",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/37018,
    title ="Ages, Irradiation History, and Chemical Composition of Lunar Rocks from the Sea of Tranquillity",
    author = "Albee, A. L. and Burnett, D. S.",
    journal = "Science",
    volume = "167",
    number = "3918",
    pages = "463-466",
    month = "January",
    year = "1970",
    
    issn = "0036-8075",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20130220-113109469",
    note = "© 1970 American Association for the Advancement of Science.\n\n\nWe thank our fellow inmates Pai Young and Uwe Derksen for the sophisticated skill and knowledge they have brought to this study, without which this work would not have been\naccomplished. We also acknowledge the unstinting efforts of J. Brown, H. L. Derksen, L. llay, and T. Wen. This work was supported by NASA contract 64049.",
    revision_no = "11",
    abstract = "The ^(87)Rb-^(87)Sr internal isochrons for five rocks yield an age of 3.65±0.05 × 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 × 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 × 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. ",
}
@article {CaltechAUTHORS_https://authors.library.caltech.edu/id/eprint/51502,
    title ="Migration of radiogenic strontium during metamorphism",
    author = "Wasserburg, G. J. and Albee, A. L.",
    journal = "Journal of Geophysical Research",
    volume = "69",
    number = "20",
    pages = "4395-4401",
    month = "October",
    year = "1964",
    doi = "10.1029/JZ069i020p04395",
    issn = "0148-0227",
    
    url = "https://resolver.caltech.edu/CaltechAUTHORS:20141110-110243393",
    note = "Copyright 1964 by the American Geophysical Union. \n\n(Manuscript received April 20, 1964; revised July 2, 1964.) \n\nWe would like to thank Mr. B. Troxel of the California Bureau of Mines for his very kind efforts in obtaining some samples of diabase. \n\nThis work was supported by grants from the National Science Foundation and the Atomic Energy Commission. \n\nContribution 1256, Division of Geological Sciences, California Institute of Technology, Pasadena.",
    revision_no = "9",
    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.",
}