Constraints on the composition and petrogenesis of the Martian crust

By H. McSween, T. Grove, M. Wyatt. 2003

155 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/c68d942b64b4ff02d5df1b5e96376a51b80908d5

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In Astronomy and Astrophysics

1. Michael D. Smith
2. Michael J. Wolff
3. L. Elkins‐Tanton
4. R. Clancy
5. Philip R. Christensen
6. J. Bibring
7. Scott L. Murchie
8. J. F. Mustard

In Atmospheric Science

1. Michael D. Smith
2. L. Elkins‐Tanton
3. Michael J. Wolff
4. R. Clancy
5. E. Parmentier
6. P. C. Hess
7. Philip R. Christensen
8. R. Arvidson

Citations in the corpus

• A petrogenetic model for the origin and compositional variation of the martian basaltic meteorites (2003, background): “However, the precision of these measurements is not sufficient at present to obtain reliable estimates of the composition of the martian crust, although much progress has been made in recent years (McSween et al. 2003).”
• Mineralogical constraints on the high-silica martian surface component observed by TES (2005, background): “The fact that alkalis do not directly result in observable thermal emission spectral features in clays or glasses suggests that spectrally derived chemistries (e.g., Hamilton et al., 2001; McSween et al., 2003; Wyatt et al., 2004b) could be in error with regard to alkali abundances.”
• EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, background): “Furthermore, near-surface Martian materials may have been chemically altered or weathered (Kirkland et al. 2003, McSween et al. 2003, Taylor et al. 2003), which further complicates the interpretation of their chemistry.”
• Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO) (2007, background): “How did Martian volcanism evolve with time, as evidenced by superposed units of different age? Martian meteorites provide evidence of extensive igneous differentiation [McSween et al., 2003].”
• Martian surface mineralogy from Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité on board the Mars Express spacecraft (OMEGA/MEx): Global mineral maps (2007, background): “[45] As mentioned previously, another model to explain Si-rich minerals could be a palagonization of basalt [Morris et al., 2003] or similarly partial weathering of surface type I rocks [McSween et al., 2003].”
• Possible formation of ancient crust on Mars through magma ocean processes (2005, result): “The TES surface type 1 [McSween et al., 2003] is a closer fit to the magmas produced by the deeper melting event in our models (Figure 8) and is found in the northern lowlands, consistent with the hypothesis that the crustal dichotomy may be formed by endogenic magma ocean processes.”
• Crustal evolution and the temporality of anorthosites (2017, background): “The martian crust appears to be vastly dominated by basaltic rocks, and the minor amounts of more evolved siliceous rocks (McSween et al., 2003) may represent products of chemical weathering (Wyatt et al., 2004).”
• The age of the martian meteorite Northwest Africa 1195 and the differentiation history of the shergottites (2007, background): “…differences have been interpreted to reflect either varying degrees of assimilation of martian crust (e.g., Jones, 1989; Borg et al., 1997; Herd et al., 2002; McSween et al., 2003), or that they have been inherited from their mantle source regions (e.g., Borg et al., 2003; Borg and Draper, 2003).”