Ages and Geologic Histories of Martian Meteorites

By L. Nyquist, D. Bogard, Chin-Yu Shih, A. Greshake, D. Stöffler, O. Eugster. 2001

642 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0aac9eeba3a2723218cfef752fc93ba1d3ae59e2

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In Aerospace Engineering

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

In Astronomy and Astrophysics

1. H. McSween
2. V. Hamilton
3. Philip R. Christensen
4. F. Nimmo
5. J. Bandfield
6. James W. Head III
7. Mark A. Wieczorek
8. M. Gudel

Citations in the corpus

• The age of SNC meteorites and the antiquity of the Martian surface (2005, neutral): “[12,13], and others.”
• Ventilation of CO2 from a reduced mantle and consequences for the early Martian greenhouse (2008, background): “5 Ga (Nyquist et al., 2001) and therefore dates from the earliest history of Mars.”
• Outgassing History and Escape of the Martian Atmosphere and Water Inventory (2015, methodology): “The crystallization ages and ejection ages of the meteorites are taken from Nyquist et al. (2001) and for ALH 84001 from Turner et al. (1997).”
• Biologically Controlled Mineralization in Prokaryotes (2003, background): “5 billion years old (Nyquist et al. 2001; Thomas-Keprta et al. 2002), contains magnetite crystals that are cuboid, teardrop, and irregular in shape with sizes ranging from about 10 to 100 nm (McKay et al.”
• Constraints on the Martian lithosphere from gravity and topography data and implication for volcanism and possible mantle heterogeneities (2005, methodology): “To date, only a few localized admittance studies have been applied to Mars using recent Mars Global Surveyor (MGS) data.”
• Heterogeneous distribution of H2O in the Martian interior: Implications for the abundance of H2O in depleted and enriched mantle sources (2016, background): “The nakhlites and chassignites also have similarly depleted radiogenic isotopic compositions (Jagoutz 1996; Shih et al. 1998, 1999, 2006; Nyquist et al. 2001; Caro et al. 2008; Carlson and Boyet 2009) that are distinct from the depleted shergottites (Nyquist et al. 1991; Borg et al. 1997, 2003;…”
• 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): “Martian meteorites, with the exception of ALH 84001, are relatively young, with crystallization ages ranging from 175 Ma to 1.3 Ga (Nyquist et al. 2001 and references therein).”
• Constraints on the composition and petrogenesis of the Martian crust (2003, background): “[9] The other Martian meteorites, collectively called SNCs (an acronym for shergottite, nakhlite, chassignite), have young crystallization ages, ranging from 175 to 1300 Ma [Nyquist et al., 2001].”
• Petrology on Mars (2015, background): “…Hesperian, ~3.65 Ga and <~3.7 Ga, respectively), based on crater counting (Parker et al. 2010; Thomson et al. 2011) than most martian meteorites (Nyquist et al. 2001; Righter et al. 2014): shergottite ages are 170–475 Ma (late Amazonian), nakhlites/chassignites are ~1.3 Ga (middle Amazonian),…”
• THE IMPORTANCE OF SECONDARY CRATERING TO AGE CONSTRAINTS ON PLANETARY SURFACES (2006, background): “The discoveries on Earth of meteorites from the Moon (Warren et al. 1983) and Mars (reviewed by Nyquist et al. 2001) indicate that distant secondary craters on these bodies must be significant.”
• Emplacement of the youngest flood lava on Mars: A short, turbulent story (2010, background): “These are all mafic–ultramafic igneous rocks, with several likely to be from young lava flows (e.g., Nyquist et al., 2001).”
• 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).”
• Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, background): “…isotopic data (Boyet and Carlson 2005) and Hf-W isotope chronometry of meteoritic material, which predicts a short time of ≈10 Myr for the main growth stage of terrestrial planets in the Solar System (e.g., Lugmair and Shukolyukow 1998; Nyquist et al. 2001; Yin et al. 2002; Kleine et al. 2002).”