The Accretion, Composition and Early Differentiation of Mars

By A. Halliday, H. Wänke, J. Birck, R. N. Clayton. 2001

156 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/8a975c7ba361cee88cd78c8ab031ccc943083e02

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In Astronomy and Astrophysics

1. L. Elkins‐Tanton
2. F. Nimmo
3. E. Parmentier
4. J. Roberts
5. Shijie Zhong
6. P. C. Hess
7. Doris Breuer
8. M. Gudel

In Atmospheric Science

1. L. Elkins‐Tanton
2. E. Parmentier
3. P. C. Hess
4. Shijie Zhong
5. J. Roberts
6. F. Nimmo
7. Japan.
8. Tilman Spohn

Citations in the corpus

• Crustal recycling, mantle dehydration, and the thermal evolution of Mars (2010, unknown): “5 Gyr [2].”
• The age of Dar al Gani 476 and the differentiation history of the martian meteorites inferred from their radiogenic isotopic systematics (2003, background): “The samples analyzed so far have recalculated W 182 values from 2.2 to 4.9, too broad a range to be caused solely by core-mantle differentiation (Snyder et al., 2000; Halliday et al., 2001).”
• Early plate tectonics versus single-plate tectonics on Mars: Evidence from magnetic field history and crust evolution (2003, methodology): “Cosmochemical data require early mantle differentiation to explain the 182Hf-182W [Lee and Halliday, 1997; Halliday et al., 2001] and other isotope data [e.g., Shih et al., 1982; Chen and Wasserburg, 1986; Jagoutz, 1991; Borg et al., 1997] of the SNCmeteorites.”
• Degree-1 convection in the Martian mantle and the origin of the hemispheric dichotomy (2006, methodology): “Our cases P1 and P2 show this pattern (Figures 1a and 1b) and support the earlier work [Harder and Christensen, 1996; Harder, 2000]. [48] When a moderate temperature dependence is used as in case P3, the convective pattern looks much different (Figure 1c). The precise reason for this is not well und”
• Magma oceans in the inner solar system (2012, background): “Similar extents of melting are subsequently expected in the large terrestrial planets owing to the conversion of kinetic energy to heat during energetic accretionary impacts with planetary embryos (e.g., Safronov 1969, Wetherill 1980, Tonks & Melosh 1993, Halliday et al. 2001).”
• Thermal evolution of the Martian core: Implications for an early dynamo (2004, background): “However this explanation is rather ad hoc, as strong evidence for an episode of plate tectonics is lacking (Pruis and Tanaka, 1995; Zuber, 2001; Halliday et al., 2001) and the timing of the interpreted transition to a stagnant lid regime is arbitrary and chosen to correlate with the apparent ;500…”
• Magma ocean fractional crystallization and cumulate overturn in terrestrial planets: Implications for Mars (2003, background): “Perovskite stability is dependent on the bulk composition, temperature, and pressure in the deep mantle, and these are not well enough constrained for Mars to make an unequivocal prediction (e.g., Longhi et al. 1992; Bertka and Fei 1998a; Halliday et al. 2001).”
• The composition of Mars (2019, methodology): “Many studies use a similar approach (Longhi et al., 1992; Halliday et al., 2001; Taylor, 2013).”
• EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, background): “Furthermore, plate tectonics on Earth provides an efficient way of mixing and rehomogenizing at least the upper mantle (e.g., Carlson 1994); the heterogeneous nature of the Martian mantle (Halliday et al. 2001) suggests that no such mixing took place.”
• Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, background): “3, and involve part or even the entire silicate mantle (e.g. Urey 1955; Safronov 1969; Wetherill 1980; LaTourrette and Wasserburg 1998; Solomatov 2000; Halliday et al. 2001; Reese and Solomatov 2006; Albarède and Blichert-Toft 2007; Bouhifd and Jephcoat 2011; Elkins-Tanton 2008, 2011, 2012).”