Rotational normal modes of Mars, their resonances, and their amplitudes

Details Rotational normal modes of Mars, their resonances, and their amplitudes Rotational normal modes of Mars, their resonances, and their amplitudes

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....1468d&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #1468

Computer Science

Scientific paper

The planet Mars is ellipsoidal and has most probably a liquid outer core. The existence of an inner core is questionable. In such a planet with a liquid core, two to four rotational normal modes are possible, two of them in the diurnal frequency band (the Free Core Nutation and the Free Inner Core Nutation) and two of them in a range of periods of a couple or a few hundreds of days (the Chandler Wobble and the Inner Core Wobble), in a frame tied to the planet. These normal modes induce resonances in, respectively the nutations and the polar motion. Free modes are most probably excited by the atmosphere of Mars to an observable level. We have developed a theoretical approach to compute the response to a random excitation and computed the effects of the atmosphere from the output of a global circulation model.

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