Ancient heat flow, crustal thickness, and lithospheric mantle rheology in the Amenthes region, Mars

Ruíz, Javier; Fernández, Carlos; Gómez-Ortíz, David; Dohm, J. M.; López, Valle; Tejero, Rosa

doi:10.1016/j.epsl.2008.02.015

Cited by 41 publications

(87 citation statements)

References 69 publications

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“…The use of a "standard" wet diabase for the Martian crust is consistent with extensive evidence for water-related geologic activity in early Mars (e.g., Fairén et al, 2003). For strain rates, we use values of 10 − 16 s − 1 and 10 − 19 s − 1 , a range usually considered for Mars (e.g., McGovern et al, 2004;Ruiz et al, 2008).…”

Section: Geophysical Investigationmentioning

confidence: 83%

“…This relation has been previously used in order to calculate surface heat flows for several regions of Mars (e.g., Solomon and Head, 1990;Zuber et al, 2000;McGovern et al, 2004;Grott et al, 2005;Ruiz et al, 2006;Kronberg et al, 2007;Ruiz et al, 2008). Moreover, the use of crustal heat sources in this kind of calculation increases the obtained heat flow values and potentially constrains crustal thickness estimates (Ruiz et al, 2006(Ruiz et al, , 2008. Thus, we calculate surface heat flows from the best-fit effective elastic thicknesses and crustal densities obtained for Claritas rise (Fig.…”

Section: Geophysical Investigationmentioning

confidence: 99%

“…The link to heat flow comes from the dependence of the ductile strengths on the temperature profile. For details on the implementation of the methodology used here, please see Ruiz et al (2008). Temperature profiles in the crust are calculated by assuming heat sources homogeneously distributed.…”

Section: Geophysical Investigationmentioning

confidence: 99%

“…Finally, for the topography curvature, we use values of 2 and 7 × 10 − 7 m − 1 , which limit a range including the majority of values published for Mars (e.g., Grott et al, 2005;Ruiz et al, 2006;Kronberg et al, 2007;Ruiz et al, 2008). Fig.…”

Section: Geophysical Investigationmentioning

confidence: 99%

“…After the crustal model of Neumann et al (2004), the crust at the Claritas rise is~80 km thick. These authors assumed a mean thickness of 45 km for the Martian crust, whereas Wieczorek and Zuber (2004), by simultaneously considering several geophysical and geochemical considerations, constrained the average thickness of the crust to be between 38 and 62 km, and Ruiz et al (2008), through calculations of heat flows from the effective elastic thickness and faulting depth for the Amenthes region, found an average thickness of~45-65 km if the crustal density is taken as 2900 kg m − 3 . Thus, for the average crustal density value used in the model of Neumann et al (2004), the crustal thickness beneath Claritas rise would be between~75 and~100 km, which further constrain the effective elastic thickness to be lower than 23 km.…”

Section: Geophysical Investigationmentioning

confidence: 99%

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Claritas rise, Mars: Pre-Tharsis magmatism?

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Section: Geophysical Investigationmentioning

confidence: 83%

Section: Geophysical Investigationmentioning

confidence: 99%

Section: Geophysical Investigationmentioning

confidence: 99%

Section: Geophysical Investigationmentioning

confidence: 99%

Section: Geophysical Investigationmentioning

confidence: 99%

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Preservation of Midlatitude Ice Sheets on Mars

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Excess ice with a minimum age of tens of millions of years is widespread in Arcadia Planitia on Mars, and a similar deposit has been found in Utopia Planitia. The conditions that led to the formation and preservation of these midlatitude ice sheets hold clues to past climate and subsurface structure on Mars. We simulate the thermal stability and retreat of buried excess ice sheets over 21 Myr of Martian orbital solutions and find that the ice sheets can be orders of magnitude older than the obliquity cycles that are typically thought to drive midlatitude ice deposition and sublimation. Retreat of this ice in the last 4 Myr could have contributed ~6% of the volume of the north polar layered deposits (NPLD) and more than 10% if the NPLD are older than 4 Myr. Matching the measured dielectric constants of the Arcadia and Utopia Planitia deposits requires ice porosities of ~25–35%. We model geothermally driven vapor migration through porous ice under Martian temperatures and find that Martian firn may be able to maintain porosity for timescales longer than we predict for retreat of the ice.

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Hemispheric Dichotomy in Lithosphere Thickness on Mars Caused by Differences in Crustal Structure and Composition

et al. 2018

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Estimates of the Martian elastic lithosphere thickness suggest small values of ∼25 km during the Noachian for the southern hemisphere and a large present‐day difference below the two polar caps (≥300 km in the north and >110 km in the south). In addition, young lava flows suggest that Mars has been volcanically active up to the recent past. We run Monte Carlo simulations using a 1‐D parameterized thermal evolution model to investigate whether a north/south hemispheric dichotomy in crustal properties and composition can explain these constraints. Our results suggest that 55–65% of the bulk radioelement content are in the crust, and most of it (43–51%) in the southern one. The southern crust can be up to 480 kg/m3 less dense than the northern one and might contain a nonnegligible proportion of felsic rocks. Our models predict a dry mantle and a wet or dry crustal rheology today. This is consistent with a mantle depleted in radioelements and volatiles. We retrieve north/south surface heat flux of 17.1–19.5 mW/m2 and 24.8–26.5 mW/m2, respectively, and a large difference in lithospheric temperatures between the two hemispheres (170–304 K in the shallow mantle). This difference could leave a signature in the seismic signals measured by the future InSight mission.

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Ancient heat flow, crustal thickness, and lithospheric mantle rheology in the Amenthes region, Mars

Cited by 41 publications

References 69 publications

Claritas rise, Mars: Pre-Tharsis magmatism?

Claritas rise, Mars: Pre-Tharsis magmatism?

Preservation of Midlatitude Ice Sheets on Mars

Hemispheric Dichotomy in Lithosphere Thickness on Mars Caused by Differences in Crustal Structure and Composition

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