Density and Seismic Profiles of the Martian Crust in the Event of an Extra-Low Temperature Gradient

Details Density and Seismic Profiles of the Martian Crust in the Event of an Extra-Low Temperature Gradient Density and Seismic Profiles of the Martian Crust in the Event of an Extra-Low Temperature Gradient

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998sosyr..32...14b&link_type=abstract

Solar System Research, vol. 32, p. 14 (1998)

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Scientific paper

When constructing models of the internal structure of Mars, Sohl and Spohn (1997) assumed a temperature gradient of about 2 K/km. Such low temperatures in the planet's crust were not considered previously. In this work, the physicopetrological structure of the crust which corresponds to this thermal model is calculated. The calculation technique and the chemical model of the crust are identical to those used in our previous work (Babeiko and Zharkov, 1997). The crust density rho reaches a value of about 3.5 g/cm3 , characteristic of the mantle at a depth of 50-100 km, thus limiting the maximum values of the crust thickness in the models under consideration. Another important feature of crust models with extra-low temperature gradients is the absence of zones of reduced seismic-wave velocities.

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