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Evolution of icy satellites

Schubert, G. and Hussmann, H. and Lainey, V. and Matson, D.L. and McKinnon, W.B and Sohl, F. and Sotin, C. and Tobie, G. and Turrini, D. and VanHoolst, T. (2010) Evolution of icy satellites. Space Science Reviews, 153 (1-4), pp. 447-484. Springer. DOI: 10.1007/s11214-010-9635-1.

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Evolutionary scenarios for the major satellites of Jupiter, Saturn, Neptune, and Pluto-Charon are discussed. In the Jovian system the challenge is to understand how the present Laplace resonance of Io, Europa, and Ganymede was established and to determine whether the heat being radiated by Io is in balance with the present tidal dissipation in the moon. In the Saturnian system, Enceladus and Titan are the centers of attention. Tidal heating is the likely source of activity at the south pole of Enceladus, although the details of how the heating occurs are not understood. An evolutionary scenario based on accretion and internal differentiation is presented for Titan, whose present substantial orbital eccentricity is not associated with any dynamical resonance. The source and maintenance of methane in Titan’s present atmosphere remain uncertain. Though most attention on the Saturnian moons focuses on Titan and Enceladus, the mid-size satellites Iapetus, Rhea, Tethys, and the irregular satellite Phoebe also draw our interest. An evolutionary scenario for Iapetus is presented in which spin down from an early rapidly rotating state is called upon to explain the satellite’s present oblate shape. The prominent equatorial ridge on Iapetus is unexplained by the spin down scenario. A buckling instability provides another possible explanation for the oblateness and equatorial ridge of Iapetus. Rhea is the only medium-size Saturnian satellite for which there are gravity data at present. The interpretation of these data are uncertain, however, since it is not known if Rhea is in hydrostatic equilibrium. Pluto and Charon are representative of the icy dwarf planets of the Kuiper belt. Did they differentiate as they evolved, and do either of them have a subsurface liquid water ocean? New Horizons might provide some answers when it arrives at these bodies.

Document Type:Article
Title:Evolution of icy satellites
AuthorsInstitution or Email of Authors
Schubert, G.Department of Earth and Space Sciences, University of California, Los Angeles, CA, USA
Hussmann, H.hauke.hussmann@dlr.de
Lainey, V.Institut de Mécanique Céléste et de Calcul de Ephémérides, Paris, France
Matson, D.L.Jet Propulsion Laboratory, Pasadena, CA
McKinnon, W.BWashington University, St. Louis
Sohl, F.frank.sohl@dlr.de
Sotin, C.Jet Propulsion Laboratory, Pasadena, CA
Tobie, G.Laboratoire de Planétologie et Géodynamique, Nantes, France
Turrini, D.INAF—Istituto di Fisica dello Spazio Interplanetario, Via Fosso del Cavaliere 100, 00133 Roma, Italy
VanHoolst, T.Royal Observatory of Belgium, Brussels, Belgium
Date:June 2010
Journal or Publication Title:Space Science Reviews
Refereed publication:Yes
In Open Access:No
In ISI Web of Science:Yes
Page Range:pp. 447-484
Keywords:Outer planet moons, icy satellites, evolution, Io, Europa, Enceladus, Dione, Titan, Iapetus, Rhea, Tethys, Phoebe, Pluto
HGF - Research field:Aeronautics, Space and Transport (old)
HGF - Program:Space (old)
HGF - Program Themes:W EW - Erforschung des Weltraums
DLR - Research area:Space
DLR - Program:W EW - Erforschung des Weltraums
DLR - Research theme (Project):W - Vorhaben Vergleichende Planetologie (old)
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Planetary Physics
Institute of Planetary Research > Planetary Geodesy
Deposited By: Frank Sohl
Deposited On:02 Nov 2010 11:02
Last Modified:26 Mar 2013 13:20

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