HR: 14:40h
AN: G53C-05    [Abstracts]
TI: Mars Polar Motion at Short Time-Scale.
AU: * Dehant, V M
EM: v.dehant@oma.be
AF: Royal Observatory of Belgium, 3 avenue Circulaire, Brussels, B1180 Belgium
AU: de Viron, O
EM: O.deviron@oma.be
AF: Royal Observatory of Belgium, 3 avenue Circulaire, Brussels, B1180 Belgium
AU: de Viron, O
EM: O.deviron@oma.be
AF: IPGP Paris 7, Place Jussieu, Paris, F75005 France
AU: Karatekin, O
EM: O.Karatekin@oma.be
AF: Royal Observatory of Belgium, 3 avenue Circulaire, Brussels, B1180 Belgium
AU: Van Hoolst, T
EM: t.vanhoolst@oma.be
AF: Royal Observatory of Belgium, 3 avenue Circulaire, Brussels, B1180 Belgium
AB: The rotation of Mars is not constant in time and presents irregularities that are mostly associated with the seasonal CO2 mass exchange between Mars' atmosphere and polar caps. This large mass redistribution (about a third of the total atmospheric mass is considered to be exchanged) induces variations in Mars' rotation speed as well as in polar motion. The effects of the atmosphere on the rotation can be estimated by using the angular momentum approach: because of conservation of angular momentum of Mars (solid body and atmosphere), considered as isolated, any change in the angular momentum of the atmosphere is associated with an opposite change in the angular momentum of the solid body of the planet. Mars' polar motion is computed for Mars models with three homogeneous layers (solid inner core, fluid outer core, and mantle) for different excitation causes (atmosphere, ice caps, and quakes). We estimate the amplitude of the polar motion resulting from atmospheric excitation, for a reasonable interval of damping factor values, for the two polar motion normal modes, i.e. the Chandler wobble and the Inner Core wobble. We show how the amplitude of the CW excited by the atmospheric noise can be interpreted in terms of anelasticity of the Martian mantle, through the CW damping factor. The damping is estimated from the observation of the mode itself under hypotheses on the type of forcing noise. We show that the signature of the inner core in the polar motion is very small, and is unlikely to be detected with the present observational precision. We further investigate the possibility to excite these normal modes through Marsquakes, and show that the predicted quake moments are not large enough to excite polar motion to an observable level. The analysis of polar motion, and in particular the determination of its normal mode components, is promising because normal mode periods and amplitudes are directly related to the properties of the deep interior. The precision needed to get useful information is very demanding, and requires improvement of the Martian rotation measurements. A first step could be the deployment of a long-lived network of landers at the Martian surface.
DE: 1213 Earth's interior: dynamics (1507, 7207, 7208, 8115, 8120)
DE: 1218 Mass balance (0762, 1223, 1631, 1836, 1843, 3010, 3322, 4532)
DE: 1221 Lunar and planetary geodesy and gravity (5417, 5450, 5714, 5744, 6019, 6250)
SC: Geodesy [G]
MN: Fall Meeting 2005