The rocks of Mars, from far and near

By H. McSween. 2002

144 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/234ba0eed70e0553058186d6dc1b00331f15b327

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In Astronomy and Astrophysics

1. V. Hamilton
2. H. McSween
3. Philip R. Christensen
4. J. Bandfield
5. James W. Head III
6. T. Grove
7. M. Wyatt
8. F. Nimmo

In Atmospheric Science

1. V. Hamilton
2. J. Bandfield
3. M. Carr
4. Philip R. Christensen
5. F. Nimmo
6. James W. Head III
7. H. McSween
8. T. Grove

Citations in the corpus

• Constraints on the composition and petrogenesis of the Martian crust (2003, methodology): “…be used to distinguish well-crystalline clay minerals from high-silica volcanic glass; however, this region was excluded by Bandfield et al. [2000] while deriving the TES spectral end-members because the CO2 atmosphere of Mars is largely opaque near this spectral region [Wyatt and McSween, 2002].”
• Geologic history of Mars (2010, background): “…tens of millions of years for volcanic surfaces in Tharsis and Elysium (Berman and Hartmann, 2002), and crystallization ages as young as 150 My from martian meteorites (McSween, 2002), suggest that Mars is still episodically active, although at low rates averaged over hundreds of millions of years.”
• EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, background): “More in-depth summaries can be found in Nyquist et al. (2001), Wanke et al. (2001), McSween (2002), and McSween et al. (2003).”
• Stability of hydrous minerals on the martian surface (2003, unknown): “…of water in past on Mars (Head et al., 1999), coupled with data sugg ing the existence of saline waters and saline–alkaline min deposits (e.g., Clark, 1978; Forsythe and Zimbelman, 1 McSween, 2002), make it distinctly possible that zeolite the clinoptilolite group formed in the past on Mars.”
• Identification of quartzofeldspathic materials on Mars (2004, background): “Martian meteorites (basaltic shergottites) with trace element and radiogenic isotope compositions suggesting crustal assimilation are not enriched in silica [ McSween, 2002 ].”
• Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars (2003, background): “…component (surface type 1), crystalline hematite, and/or a component (surface type 2) that was identified as basaltic andesite, andesite, or partially weathered basalt (Bandfield et al. 2000; Christensen et al. 2000a; Christensen et al. 2000b; Hamilton et al. 2001c; Wyatt and McSween 2002).”
• Sedimentary silica on Mars (2003, unknown): “Keywords: geochemistry, Mars, silica, thermal emission.”
• Ejection of Martian meteorites (2005, background): “The real density of ALH 77005 was estimated to be 2830–2890 kg/m3 (McSween 2002).”