The Bulk Composition, Mineralogy and Internal Structure of Mars

Longhi, J.; Knittle, Elise; Holloway, John; Waenke, H.

doi:10.2307/j.ctt207g59v.10

Cited by 119 publications

(160 citation statements)

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“…We suggest that the extraction of this crustal component, with melting of garnet in the mantle (Longhi et al 1992), is likely the event that depleted the martian mantle in Al. The mean martian crustal thickness is about 50 km, which is a significant fraction of Mars' volume (4%; Zuber et al 2000) and represents a significant amount of volcanism that could produce a depleted mantle.…”

Section: Integrating Martian Meteorites and Martian Geologymentioning

confidence: 99%

Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars

Hamilton

Christensen

McSween

et al. 2003

Meteorit & Planetary Scien

162

165

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Abstract-The objective of this study was to identify and map possible source regions for all 5 known martian meteorite lithologies (basalt, lherzolite, clinopyroxenite, orthopyroxenite, and dunite) using data from the Mars Global Surveyor Thermal Emission Spectrometer (MGS TES). We deconvolved the TES data set using laboratory spectra of 6 martian meteorites (Los Angeles, Zagami, ALH A77005, Nakhla, ALH 84001, and Chassigny) as end members, along with atmospheric and surface spectra previously derived from TES data. Global maps (16 pixels/degree) of the distribution of each meteorite end member show that meteorite-like compositions are not present at or above TES detectability limits over most of the planet's dust-free regions. However, we have confidently identified local-scale (100s-1000s km 2 ) concentrations of olivine-and orthopyroxene-bearing materials similar to ALH A77005, Chassigny, and ALH 84001 in Nili Fossae, in and near Ganges Chasma, in the Argyre and Hellas basin rims, and in Eos Chasma. Nakhla-like materials are identified near the detection limit throughout the eastern Valles Marineris region and portions of Syrtis Major. Basaltic shergottites were not detected in any spatially coherent areas at the scale of this study. Martian meteorite-like lithologies represent only a minor portion of the dust-free surface and, thus, are not representative of the bulk composition of the ancient crust. Meteorite-like spectral signatures identified above TES detectability limits in more spatially restricted areas (

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Section: Integrating Martian Meteorites and Martian Geologymentioning

confidence: 99%

Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars

Hamilton

Christensen

McSween

et al. 2003

Meteorit & Planetary Scien

162

165

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“…Mars is more iron-rich than the Earth (Longhi et al, 1992; Table 2 in Robinson and Taylor, 2001), 125…”

Section: Mantle 121mentioning

confidence: 99%

Seismological implications of a lithospheric low seismic velocity zone in Mars

Zheng

Nimmo

Lay

2015

Physics of the Earth and Planetary Interiors

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“…1), while the gas disk that would have produced the drag is believed to have survived only a few million, this would not have altered the apparent metallicity of the Sun. Longhi et al 1992 ; for Jupiter and Saturn from Guillot 1999b ; for Uranus from Podolak et al 1991 ; for Neptune from Hubbard et al 1995. For the gas giants, we take representative values for the heavy-element mass ; the typical uncertainty is roughly^30%.…”

Section: Pollution By Small Bodies In Our Solar Systemmentioning

confidence: 99%

Stellar Pollution in the Solar Neighborhood

Murray

Chaboyer

Arras

et al. 2001

ApJ

107

127

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We study spectroscopically determined iron abundances of 640 solar-type stars to search for the signature of accreted iron-rich material. We Ðnd that the metallicity [Fe/H] of a subset of 466 main-sequence stars, when plotted as a function of stellar mass, mimics the pattern seen in lithium abundances in open clusters. Using Monte Carlo models, we Ðnd that, on average, these stars appear to have accreted D0.5 of iron while on the main-sequence. A consistency check is provided by a much smaller sample of M1 9 stars in the Hertzsprung gap, which are slightly evolved and the convection zones of which are signiÐ-cantly more massive ; they have lower average [Fe/H], and their metallicity shows no clear variation with stellar mass. We argue that our Sun is likely to have accreted a similar amount of iron ; in this respect, most systems resemble ours rather than the currently known extrasolar planetary systems. These Ðndings suggest that terrestrial-type material is common around solar-type stars.

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The Bulk Composition, Mineralogy and Internal Structure of Mars

Cited by 119 publications

References 0 publications

Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars

Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars

Seismological implications of a lithospheric low seismic velocity zone in Mars

Stellar Pollution in the Solar Neighborhood

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