Thermal and crustal evolution of Mars

By S. Hauck,, Roger J. Phillips. 2002

295 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/53f7bf9d65245a669c6229893c0ed84f52c55d1d

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Citations in the corpus

Ventilation of CO2 from a reduced mantle and consequences for the early Martian greenhouse (2008, background): “Ventilation of mantle CO2 through time can be estimated from constraints or models of magmatic output (Craddock and Greeley, 1995; Jakosky and Shock, 1998; Carr, 1999; Phillips et al., 2001; Hauck and Phillips, 2002; Manning et al., 2006; O'Neill et al., 2007).”
The bulk composition of Mars (2013, background): “For example, K and Th do not readily fractionate, as shown by their similar, and very low ( 1), crystal-melt partition coefficients (Beattie, 1993; Borg and Draper, 2003; Hauri et al., 1994).”
Geologic history of Mars (2010, background): “According to Hauck and Phillips (2002), heat flows would have peaked at 60–70 mW m − 2 around 4.4 Gyr ago, and then declined almost linearly to a present value of not more than 10–20 mW m − 2 , and possibly much lower, as indicated by the lack of flexure of the lithosphere under the present polar…”
Thickness of the Martian crust: Improved constraints from geoid-to-topography ratios (2004, methodology): “In addition, a recent thermal evolution study by Hauck and Phillips [2002] has highlighted the fact that the thickness of the Martian crust can help discriminate between different estimates of the bulk concentration of heat-producing elements in this planet, as well as the rheology of the mantle w”
Constraints on the composition and petrogenesis of the Martian crust (2003, background): “Thermal models suggest that the stagnant lid model operating during the entire Martian evolution can more readily explain the volume and timing of crust formation than can a model of early plate tectonics followed by a stagnant lid [Hauck and Phillips, 2002; Breuer and Spohn, 2003].”
Very recent and wide‐spread basaltic volcanism on Mars (2011, background): “Indeed, thermal evolution models of Mars suggest that volcanism should have stopped at least some hundred million years ago [ Hauck and Phillips, 2002; Breuer and Spohn, 2003].”
EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, background): “Second, the efficient cooling also provides a way of avoiding early massive melting on Mars (Hauck & Phillips 2002).”
Thermal evolution of the Martian core: Implications for an early dynamo (2004, background): “The initial thermal state of the mantle and core is uncertain and depends on processes such as accretion, core formation, and giant impacts (Hauck and Phillips, 2002).”
Updated global map of Martian valley networks and implications for climate and hydrologic processes (2010, background): “Mars is covered with signs of magmatism/volcanism, and the heat flux on early Mars was likely a factor of 2 to 3 higher than at present [e.g., Hauck and Phillips, 2002 ].Phillips et al.[2001] showedthatthemajorityoftheTharsiscomplexformedinthe Noachian epoch.”
Sulfur's impact on core evolution and magnetic field generation on Ganymede (2005, methodology): “A preliminary study utilized a liquidus with a nonlinear dependence on mass fraction of sulfur [Hauck et al., 2002], but given the lack of relevant experimental data, this added unconstrained complexity, though plausible, is not justified.”
Outgassing History and Escape of the Martian Atmosphere and Water Inventory (2015, background): “Alternatively, numerical models of the thermochemical evolution of Mars can be used to calculate the globally averaged crustal production rates (Hauck and Phillips 2002; Breuer and Spohn 2006; Fraeman and Korenaga 2010; Morschhauser et al. 2011).”
Internal and tectonic evolution of Mercury (2003, methodology): “First, we explicitly solve the nonlinear, time-dependent, heat conduction equation in the thermal lithosphere by means of a finite element solution with adaptive remeshing [24].”
The seismicity of Mars (2020, background): “006 and Q=95±10) as described in Khan et al. (2018). Briefly, a set of Martian compositions (Dreibus & Wänke, 1984; Lodders & Fegley, 1997; Sanloup et al.”
Crustal structure of Mars from gravity and topography (2004, background): “Such a mechanism would have operated during an early period of high mantle temperature and melt production [ Hauck and Phillips , 2002].”
Bulk composition and early differentiation of Mars (2007, background): “This is consistent with Martian meteoritic isotopic data, the geologic record placing most volcanic activity before the end of the Hesperian [Tanaka et al., 1992], and thermal modeling by Hauck and Phillips [2002] .”