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  • 1
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    Record of fluid-rock interactions on Mars from the meteorite ALH84001 (1994)
    In:  Other Sources
    Details
    Publication Date: 2011-08-24
    Description: Allan Hills (ALH) 84001 is the most recently recognized member of a suite of meteorites--the SNCs--that almost certainly originated on Mars. Several factors distinguish ALH84001 from the other SNC meteorites. Preliminary studies suggest that it may be older than other martian meteorites. Moreover, it contains abundant, zoned domains of calcium-iron-magnesium carbonate that are indigenous to the sample and thus may hold important clues regarding near-surface processes on Mars and the evolution of the martian atmosphere. We report here analyses of the carbon and oxygen stable-isotope compositions of the carbonates that place constraints on their formation conditions. Our results imply the presence of at least two chemically distinct carbonates--one Ca,Fe-rich, the other Mg-rich--that are enriched in 13C relative to terrestrial carbonates (delta 13C approximately +41/1000), consistent with martian atmospheric CO2 as the carbon source. The oxygen isotope compositions of the carbonates indicate that they precipitated from a low-temperature fluid in the martian crust. Combined with textural and bulk geochemical considerations, the isotope data suggest that carbonate deposition took place in an open-system environment in which the ambient temperature fluctuated.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Nature (ISSN 0028-0836); Volume 372; 6507; 655-7
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  • 2
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    Proposed Science Requirements and Acquisition Priorities for the First Mars Sample Return (2000)
    In:  CASI
    Details
    Publication Date: 2004-12-03
    Description: A sample return mission is an important next step in the exploration of Mars. The first sample return should come early in the program time-line because the science derived from earth-based analyses of samples provides crucial "ground truth" needed for further exploration planning, enhancement of remote measurements, and achieving science goals and objectives that include: (1) the search for environments that may support life and any indicators of the past or present existence of life, (2) understanding the history of water and climate on Mars, (3) understanding the evolution of Mars as a planet. Returned samples from Mars will have unique value because they can be studied by scientists worldwide using the most powerful analytical instruments available. Furthermore, returned Mars samples can be preserved for studies by future generations of scientists using new techniques and addressing new issues in Mars science. To ensure a high likelihood of success, the first sample return strategy should be simple and focused. We outline a fundamental set of sample requirements and acquisition priorities for Mars sample return.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Concepts and Approaches for Mars Exploration; Part 1; 2; LPI-Contrib-1062
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  • 3
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    Geochemistry of Martian Meteorites and the Petrologic Evolution of Mars (2002)
    In:  CASI
    Details
    Publication Date: 2004-12-03
    Description: Mafic igneous rocks serve as probes of the interiors of their parent bodies - the compositions of the magmas contain an imprint of the source region composition and mineralogy, the melting and crystallization processes, and mixing and assimilation. Although complicated by their multifarious history, it is possible to constrain the petrologic evolution of an igneous province through compositional study of the rocks. Incompatible trace elements provide one means of doing this. I will use incompatible element ratios of martian meteorites to constrain the early petrologic evolution of Mars. Incompatible elements are strongly partitioned into the melt phase during igneous processes. The degree of incompatibility will differ depending on the mineral phases in equilibrium with the melt. Most martian meteorites contain some cumulus grains, but nevertheless, incompatible element ratios of bulk meteorites will be close to those of their parent magmas. ALH 84001 is an exception, and it will not be discussed. The martian meteorites will be considered in two groups; a 1.3 Ga group composed of the clinopyroxenites and dunite, and a younger group composed of all others.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Unmixing the SNCs: Chemical, Isotopic, and Petrologic Components of the Martian Meteorites; 37-38; LPI-Contrib-1134
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  • 4
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    Geochemistry of Martian Meteorites and the Petrologic Evolution of Mars (2002)
    In:  CASI
    Details
    Publication Date: 2004-10-05
    Description: Mafic igneous rocks serve as probes of the interiors of their parent bodies - the compositions of the magmas contain an imprint of the source region composition and mineralogy, the melting and crystallization processes, and mixing and assimilation. Although complicated by their multifarious history, it is possible to constrain the petrologic evolution of an igneous province through compositional study of the rocks. Incompatible trace elements provide one means of doing this. I will use incompatible element ratios of martian meteorites to constrain the early petrologic evolution of Mars. Incompatible elements are strongly partitioned into the melt phase during igneous processes. The degree of incompatibility will differ depending on the mineral phases in equilibrium with the melt. Most martian meteorites contain some cumulus grains, but nevertheless, incompatible element ratios of bulk meteorites will be close to those of their parent magmas. ALH 84001 is an exception, and it will not be discussed. The martian meteorites will be considered in two groups; a 1.3 Ga group composed of the clinopyroxenites and dunite, and a younger group composed of all others.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Report of the Workshop on Unmixing the SNCs: Chemical, Isotopic, and Petrologic Components of Martian Meteorites; LPI-Contrib-1153
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  • 5
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    Preliminary Examination of Sahara 99555: Mineralogy and Experimental Studies of a New Angrite (2000)
    In:  Other Sources
    Details
    Publication Date: 2017-10-02
    Description: We report mineralogy and experimental petrology of a new angrite Sahara 99555. We believe that it cooled very rapidly near the surface of its parent body and it shows a close affinities to LEW 87051 and Asuka 881371.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXI; LPI-Contrib-1000
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  • 6
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    Asteroid-Meteorite Links: The Vesta Conundrum(s) (2006)
    In:  CASI
    Details
    Publication Date: 2018-06-11
    Description: Although a direct link between the HED meteorites and the asteroid 4 Vesta is generally acknowledged, several issues continue to be actively examined that tie Vesta to early processes in the solar system. Vesta is no longer the only basaltic asteroid in the Main belt. In addition to the Vestoids of the Vesta family, the small asteroid Magnya is basaltic but appears to be unrelated to Vesta. Similarly, diversity now identified in the collection of basaltic meteorites requires more than one basaltic parent body, consistent with the abundance of differentiated parent bodies implied by iron meteorites. The timing of the formation of the Vestoids (and presumably the large crater at the south pole of Vesta) is unresolved. Peaks in Ar-Ar dates of eucrites suggest this impact event could be related to a possible late heavy bombardment at least 3.5 Gyr ago. On the other hand, the optically fresh appearance of both Vesta and the Vestoids requires either a relatively recent resurfacing event or that their surfaces do not weather in the same manner thought to occur on other asteroids such as the ordinary chondrite parent body. Diversity across the surface of Vesta has been observed with HST and there are hints of compositional variations (possibly involving minor olivine) in near-infrared spectra.
    Keywords: Lunar and Planetary Science and Exploration
    Type: IAU
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  • 7
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    Petrology, Geochemistry and Genesis of Ureilites (2005)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: Ureilites are enigmatic achondrites that have some characteristics resulting from high temperature igneous processing, yet retain other characteristics inherited from the solar nebula. They are basalt-depleted ultramafic rocks containing 7-66 mg/g elemental C. They are rich in noble gases and display a correlation between mg# and Delta (17)O. This mishmash of properties has engendered various models for ureilite genesis, from those in which nebular processes dominate to those in which parent body igneous processes dominate. Characterization of new ureilites, especially of new subtypes, is an important part of attempts to unravel the history of the ureilite parent body or bodies. Here we report on the petrology and geochemistry of a suite of ureilites, mostly from Antarctica, and use these data to discuss ureilite petrogenesis. Additional information is included in the original extended abstract.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 13; LPI-Contrib-1234-Pt-13
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  • 8
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    Petrology of New Stannern-trend Eucrites and Eucrite Genesis (2004)
    In:  CASI
    Details
    Publication Date: 2018-06-11
    Description: Eucrites are basaltic meteorites of the howardite-eucrite-diogenite (HED) suite that originated on a differentiated asteroid, possibly 4 Vesta. Basaltic eucrites are divided into three subgroups based on composition: main group, Stannern-trend, and Nuevo Laredo-trend. The main group and Nuevo Laredo-trend define a sequence formed by fractional crystallization of pigeonite and plagioclase from primitive parent melts [2, 3]. The Stannern-trend cannot be explained this way, but may rather represent a partial-melt sequence of their parent body. However, this model seems inadequate to explain eucrite siderophile element contents, and it is difficult to develop a single unifying model for petrogenesis of all eucrites. Until recently, there were only four Stannern- trend eucrites. One is an anomalous partial cumulate. There is little geochemical variation among these meteorites, so the Stannern-trend was poorly defined. Geochemical studies have identified four additional eucrites as members of the Stannern-trend; one extends the Stannern-trend closer to the main group [5]. No detailed descriptions of these rocks have been published. In order to better integrate these eucrites into the suite, we have done petrologic study of them. They are: LEW 88010, PCA 82501, PCA 91006 and PCA 91179.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Achondrites: An Awesome Assortment; LPI-Contrib-1197
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  • 9
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    The Dichotomous HED Meteorite Suite (2004)
    In:  CASI
    Details
    Publication Date: 2018-06-11
    Description: The howardite, eucrite and diogenite (HED) clan is the largest suite of crustal rocks available from a differentiated asteroid. Attempts to unravel the petrogenetic history of the HED parent body have tacitly assumed that the suite is representative of the crust, and thus can be used to understand the differentiation history of the entire parent body. This assumption is a holdover from a time when we knew little about the HED parent body. Much has changed. Is this assumption still valid? HED Geochemistry: The HED suite is composed
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Achondrites: An Awesome Assortment; LPI-Contrib-1197
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  • 10
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    Devolatilized-Allende Partial Melts as an Analog for Primitive Angrite Magmas (2004)
    In:  CASI
    Details
    Publication Date: 2018-06-11
    Description: We have shown that partial melts of devolatilized Allende chondrite (CV3) have bulk compositions generally similar to those of angrites. Here we show that the recently described D'Orbigny and Sahara 99555 angrites are virtually identical in major-element composition to specific Allende experimental melts from. This observation has petrogenetic significance for the origins of the angrite clan.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Achondrites: An Awesome Assortment; LPI-Contrib-1197
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