Physics
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf...59z&link_type=abstract
European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a
Physics
Scientific paper
For the first time the period of the Chandler Wobble was obtained in [1]. In many publications, in which the models of interior structure of Mars were constructed, there have been calculated the model values of Chandler period of about 200 days. The signature at the Chandler frequency is mixed with the nearly 1/3 Mars year mass redistribution term (229 days), and may cause the polar motion signal to shift to longer periods. Accounting this fact Konopliv et al. [1] looked for a Chandler wobble of Mars with a period of 200 to 210 days and pointed out, that it might be possible to resolve the free wobble period from the spectra with about 6 years of Odyssey Doppler data. We have constructed the suites of interior structure models with 50- and 100-km thick crust and averaged crustal density varying in the range of 2.7-3.2 g/cm3, which content new values for the moment of inertia and the elastic tidal Love number defined in [1]. The models differ in density contrast at the crust-mantle boundary and the core radius. The observational data constrain the radius of a liquid core to be within 1700-1800 km. For 50-km thick crust its density is within 3.0-3.2 g/cm k s 2 3 (an iron atomic number of mantle silicates Fe2+/((Fe2++Mg) multiplied by 100: Fe#20), 2.8-3.1 g/cm3 (Fe#22), 2.7-2.8 g/cm3 (Fe#25); for 100-km thick crust we have 3.2 g/cm3 (Fe#20), 3.1-3.2 g/cm3 (Fe#22), 3.0-3.1 g/cm3 (Fe#25). The parameters of the models are given in [3]. For all models the weight ratio Fe/Si is about 1.7. The technique of the modelling is described in detail in [2].
Gudkova T. V.
Zharkov Vladimir Naumovich
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