000006596 001__ 6596
000006596 005__ 20240122122233.0
000006596 037__ $$aCTALK-2024-0008
000006596 100__ $$aCoyette, A.
000006596 245__ $$aCassini States of Ganymede and Callisto
000006596 260__ $$c2023
000006596 269__ $$c2023-07-07
000006596 520__ $$aLike our Moon, the large icy satellites of Jupiter are thought to be in a Cassini State, an equilibrium rotation state characterized by a synchronous rotation rate and a precession rate of the rotation axis equal to that of the normal to the orbit. In these equilibrium states (up to four Cassini States are possible for a solid and rigid satellite), the spin axis of the satellite, the normal to its orbit and the normal to the inertial plane remain coplanar with an obliquity that remains theoretically constant. However, as the gravitational torque exerted on the satellite shows small periodic variations, the orientation of the rotation axis will also vary with time and nutations in obliquity will appear. Here we present the influence of the triaxiality and of the presence of a subsurface ocean on the Cassini States of Ganymede and Callisto and assess the possibility of determining whether a future observation of the obliquity of Ganymede or Callisto by the JUICE Mission could constrain the interior structure of these satellites.
000006596 536__ $$a3PRODPLANINT/$$c3PRODPLANINT/$$f3PRODPLANINT
000006596 594__ $$aNO
000006596 6531_ $$aGanymede
000006596 6531_ $$aCallisto
000006596 700__ $$aBaland, R.-M.
000006596 700__ $$aVan Hoolst, T.
000006596 773__ $$tComplex Planetary Systems II Kavli-IAU Symposium 382, Namur, Belgium
000006596 8560_ $$frose-marie.baland@ksb-orb.be
000006596 85642 $$ahttps://cpsii.unamur.be/
000006596 906__ $$aContributed
000006596 980__ $$aCTALKCONT