Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011dda....42.0204j&link_type=abstract
American Astronomical Society, DDA meeting #42, #2.04; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
The effort to determine the orientation and precession of Saturn's pole is currently motivated by three needs: to orient the Saturn gravity field for ephemeris development and spacecraft navigation, to orient the Saturn ring plane for studies of ring structure and dynamics, and to determine Saturn's polar moment of inertia for studies of Saturn's interior. Boué, G. and Laskar, J. (2006 Icarus 185, 312) published an informative theoretical discussion of polar motion applicable to Saturn. However, their model cannot be easily used in practice. Jacobson (2007 BAAS 39, 317) presented a pole model in the standard IAU trigometric series representation based on the rigid body rotational equations of motion with couples exerted by the Sun, Titan, and Iapetus. He determined the orientation and precession by fitting Saturn ring occultation measurements, in particular: the radio occultation of Voyager 1, the occultation of the star δSco seen with the Voyager 2 Ultraviolet Spectrometer, the 1989 occultation of the star 28 Sgr seen from the Earth, the 1991 occultation of the star GSC 6323-01396 seen from HST, and ring plane crossing times (Nicholson and French, 1997 BAAS 29, 1097). We have since acquired measurements from the 1995 occultation of the star GSC 5249-01240 seen from HST and the re-reduced meansurements of the 1991 occultation (French et al. 2010 AJ 139, 1649). In this paper we present our current results using the occultation data together with satellite astrometry and tracking of the Voyager and Cassini spacecraft. We also discuss future plans for the incorporation of Cassini ring occultation observations.
French Richard G.
Jacobson Robert A.
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