Other
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja......239z&link_type=abstract
EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #239
Other
Scientific paper
The problems arising at the construction of the crust, mantle and core in martian models are considered. The crust consists of about 10 km thick outer porous layer, in which the density increases from 1.6 g/cm^3 to the density of the consolidated ferrous basalts of about 3.2-3.3 g/cm^3. The crust structure depends on the temperature distribution in it (on the heat flux) and the history of its formation. The crust structure obtained under the joint interpretation of topography and gravitational field using the uniform density model crust of 2.9-3.0 g/cm^3 is not appropriate very well for the description not deep structures such as Hellas, Isidis, Utopia. Moreover, in these models the density drop at the crust-mantle boundary is almost two times larger. The mantle and core models are based on the chemical models of martian interiors: 1) the SNC meteorite model of Wánke and Dreibus (WD), 2) Oxygen isotope mixing models (OIM), which give correct isotope composition of oxygen in SNC meteorites (Lodders and Fegley, 1997; Sanloup et al., 1999). The mantle models (WD) and (OIM) are similar. They are a little different by the value of Fe#. In WD model the mantle is olivine mantle, and in OIM model the large amount of SiO_2 leads to pyroxene-olivine or pyroxene mantle. Seismic methods allow to reveal these differences. The WD and OIM models differ by the sulfur content in the core. Moreover, under martian core formation significant amount of hydrogen could enter the core (Zharkov, 1996). Seismic and other geophysical methods are enable to verify the martian models discussed at the present time. According to tidal delay of Phobos a trial model of dissipative factor Qμ for martian mantle is constructed. Our seismic models take into account the correction for dynamical shear modulus (for physical dispersion).
Gudkova T. V.
Zharkov Vladimir Naumovich
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