Influence of early plate tectonics on the thermal evolution and magnetic field of Mars

By F. Nimmo, D. Stevenson. 2000

266 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/bc2ed5c93bb9db298630dd4614d0f5329fc2f3da

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Citations in the corpus

The MAVEN Magnetic Field Investigation (2015, background): “…with or without plate 111 tectonics, for the first 0.5 – 1 Gyr [Breuer and Spohn, 2003; Schubert and Spohn, 1990; Stevenson et al., 112 1983; Connerney et al., 2004], persisting as long as the core heat flow remains above a critical threshold 113 for thermal convection [Nimmo and Stevenson, 2000].”
Crustal structure of Mars from gravity and topography (2004, background): “[83] The spatial distribution of the 32-km peak in the northern lowlands crustal thickness distribution is most simply explained by an endogenic mechanism of formation, arguably an early episode of crustal spreading [Sleep, 1994; Nimmo and Stevenson, 2000; Zuber, 2001] or a degree 1 style of mantl”
EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, background): “The high cooling rate also favors the generation of an early Martian dynamo (Nimmo & Stevenson 2000).”
Magnetic field of Mars: Summary of results from the aerobraking and mapping orbits (2001, background): “An early era of plate tectonics, with an enhanced surface heat flux, favors generation of a Mars magnetic field; the chronologies of both are intimately linked [Nimmo and Stevenson, 2000].”
Degree-1 convection in the Martian mantle and the origin of the hemispheric dichotomy (2006, background): “We expect that the CMB heat flux in Mars was close to this limit, given that it shut down fairly early [Nimmo and Stevenson, 2000].”
Thermal evolution of the Martian core: Implications for an early dynamo (2004, methodology): “…the heat flux due to thermal conduction is the maximum heat flux that can be extracted without triggering core convection and is given by (Nimmo and Stevenson, 2000): 98 GEOLOGY, February 2004 dT kag(r)TcF 5 2k 5 , (1)cond 1 2dr Cpadiabat where k is the thermal conductivity, dT/dr is the…”
Thickness of the Martian crust: Improved constraints from geoid-to-topography ratios (2004, background): “While such a scenario could plausibly lead to a core dynamo and explain the ancient crustal magnetic anomalies of this planet [Nimmo and Stevenson, 2000], plate tectonics would also efficiently cool the mantle and give rise to a thinner than observed crust [Breuer and Spohn, 2003].”
Thermal and crustal evolution of Mars (2002, background): “Such a possibility has been previously proposed for Mars [Nimmo and Stevenson, 2000] as a result of a switch in convective regime from early plate tectonics to stagnant lid.”
The effect of rheological parameters on plate behaviour in a self-consistent model of mantle convection (2004, background): “Temperatures are colour-coded between the dimensionless values of zero (blue) and one (red). candidate for such a change could be Mars which is believed to be in the stagnant lid regime today but may have shown plate tectonics earlier in its evolution (Sleep, 1994; Nimmo and Stevenson, 2000).”
Energetics of the Core (2015, background): “This result is well known (e.g. Nimmo and Stevenson 2000), but the utility of equation (77) is that it allows dynamo dissipation to be taken into account explicitly: a more strongly dissipative core requires a more superadiabatic CMB heat flow to operate.”
Conditions for the onset of plate tectonics on terrestrial planets and moons (2007, background): “, 1999) requires the existence of a dynamo on early Mars (Nimmo and Stevenson, 2000), suggesting plate-tectonics in early Martian history (Sleep, 1994; Lenardic et al.”
Early plate tectonics versus single-plate tectonics on Mars: Evidence from magnetic field history and crust evolution (2003, background): “This is a factor of about three shorter than the transition time calculated by Nimmo and Stevenson [2000]. The difference of the length of the transitional stage may be caused by the more accurate determination of the temperature profile during conductive cooling for the presented model and by the d”
Constraints on the composition and petrogenesis of the Martian crust (2003, background): “, 2002] and magnetic lineation patterns detected in parts of the ancient southern highlands [Connerney et al., 1999; Nimmo and Stevenson, 2000], although there is little or no supporting evidence [Pruis and Tanaka, 1995].”
The influence of potassium on core and geodynamo evolution (2003, background): “Rac is generally assumed to be 600 (Nimmo & Stevenson 2000).”