000005169 001__ 5169
000005169 005__ 20210125135527.0
000005169 037__ $$aPOSTER-2021-0008
000005169 100__ $$aCoyette, Alexis
000005169 245__ $$aCassini state of Galilean Moons: Influence of a subsurface ocean 
000005169 260__ $$c2020
000005169 269__ $$c2020-05-04
000005169 520__ $$aLarge moons such as the Galilean satellites are thought to be in an equilibrium rotation state, called a Cassini state (Peale, 1969). This state is characterized by a synchronous rotation and a precession rate of the rotation axis that is equal to the precession rate of the normal to its orbit. It also implies that the spin axis, the normal to the orbit and the normal to the Laplace plane are coplanar with a (nearly) constant obliquity. For rigid bodies, up to 4 possible Cassini states exist, but not all of them are stable. It is generally assumed that the Galilean satellites are in Cassini State I for which the obliquity is close to zero (see e.g. Baland et al. 2012). However, it is also theoretically possible that these satellites occupy or occupied another Cassini state. We here investigate how the interior structure, and in particular the presence of a subsurface ocean, influences the existence and stability of the different possible Cassini states.
000005169 536__ $$aProdex/$$cProdex/$$fProdex
000005169 594__ $$aNO
000005169 6531_ $$aCassini state
000005169 6531_ $$aGalilean satellites
000005169 700__ $$aBaland, Rose-Marie
000005169 700__ $$aLemaitre, Anne
000005169 700__ $$aVan Hoolst, Tim
000005169 773__ $$t22nd EGU General Assembly, held online
000005169 8560_ $$frose-marie.baland@observatoire.be
000005169 85642 $$ahttps://meetingorganizer.copernicus.org/EGU2020/EGU2020-8210.html
000005169 8564_ $$s318834$$uhttps://publi2-as.oma.be/record/5169/files/EGU2020-8210-print-1.pdf
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000005169 980__ $$aCPOSTER