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Icy Satellites: Geological Evolution and Surface Processes

Jaumann, Ralf und Clark, Roger N. und Nimmo, Francis und Hendrix, Amanda R. und Buratti, Bonnie J. und Denk, Tilmann und Moore, Jeffrey M. und Schenk, Paul M. und Ostro, Steve J. und Srama, Ralf (2009) Icy Satellites: Geological Evolution and Surface Processes. In: Saturn from Cassini-Huygens Springer. Seiten 637-681. ISBN 978-1-4020-9216-9.

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The sizes of the Saturnian icy satellites range from ~ 1;500 km in diameter (Rhea) to ~20km (Calypso), and even smaller ‘rocks’ of only a kilometer in diameter are common in the system. All these bodies exhibit remarkable, unique features and unexpected diversity. In this chapter, we will mostly focus on the ‘medium-sized icy objects’ Mimas, Tethys, Dione, Rhea, Iapetus, Phoebe and Hyperion, and consider small objects only where appropriate, whereas Titan and Enceladus will be described in separate chapters. Mimas and Tethys show impact craters caused by bodies that were almost large enough to break them apart. Iapetus is unique in the Saturnian system because of its extreme global brightness dichotomy. Tectonic activity varies widely — from inactive Mimas through extensional terrains on Rhea and Dione to the current cryovolcanic eruptions on Enceladus — and is not necessarily correlated with predicted tidal stresses. Likely sources of stress include impacts, despinning, reorientation and volume changes. Accretion of dark material originating from outside the Saturnian system may explain the surface contamination that prevails in the whole satellite system, while coating by Saturn's E-ring particles brightens the inner satellites. So far, among the surprising Cassini discoveries are the volcanic activity on Enceladus, the sponge-like appearance of Hyperion and the equatorial ridge on Iapetus — unique features in the solar system. The bright-ray system on Rhea was caused by a relatively recent medium impact which formed a ~40km crater at 12°S latitude, 112°W longitude, while the wispy streaks on Dione and Rhea are of tectonic origin. Compositional mapping shows that the dark material on Iapetus is composed of organics, CO2 mixed with H2O ice, and metallic iron, and also exhibits possible signatures of ammonia, bound water, H2 or OH-bearing minerals, and a number of as-yet unidentified substances. The spatial pattern, Rayleigh scattering effect, and spectral properties argue that the dark material on Iapetus is only a thin coating on its surface. Radar data indicate that the thickness of the dark layers can be no more than a few decimeters; this is also consistent with the discovery of small bright-ray and bright-floor craters within the dark terrain. Moreover, several spectral features of the dark material match those seen on Phoebe, Iapetus, Hyperion, Dione and Epimetheus as well as in the F-ring and the Cassini Division, implying that throughout the Saturnian system. All dark material appears to have a high content of metallic iron and a small content of nano-phase hematite. However, the complete composition of the dark material is still unresolved, and additional laboratory work is required. As previously concluded for Phoebe, the dark material appears to have originated external to the Saturnian system. The icy satellites of Saturn offer an unrivalled natural laboratory for understanding the geological diversity of different-sized icy satellites and their interactions within a complex planetary system.

Dokumentart:Beitrag in einem Lehr- oder Fachbuch
Titel:Icy Satellites: Geological Evolution and Surface Processes
AutorenInstitution oder E-Mail-AdresseAutoren-ORCID-iD
Clark, Roger N.Denver Federal Center, U.S. Geological Survey, Denver, CO 80225, USANICHT SPEZIFIZIERT
Nimmo, FrancisDepartment of Earth and Planetary Sciences, University of California Santa Cruz, Santa Cruz, CA 95064, USANICHT SPEZIFIZIERT
Hendrix, Amanda R.Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USANICHT SPEZIFIZIERT
Buratti, Bonnie J. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USANICHT SPEZIFIZIERT
Denk, TilmannInstitute of Geological Sciences, Freie Universität Berlin, Malteserstr. 74–100, Berlin, 12249, GermanyNICHT SPEZIFIZIERT
Moore, Jeffrey M.NASA Ames Research Center, MS 245-3 Moffett Field, CA 94035-1000, USANICHT SPEZIFIZIERT
Schenk, Paul M.Lunar and Planetary Institute, Houston, TX 77058, USANICHT SPEZIFIZIERT
Ostro, Steve J.Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USANICHT SPEZIFIZIERT
Srama, RalfMax Planck Institut für Kernphysik, Heidelberg, 69117, GermanyNICHT SPEZIFIZIERT
Erschienen in:Saturn from Cassini-Huygens
Referierte Publikation:Ja
In Open Access:Nein
In ISI Web of Science:Nein
Seitenbereich:Seiten 637-681
HerausgeberInstitution und/oder E-Mail-Adresse der Herausgeber
Krimigis, Stamatios M.NICHT SPEZIFIZIERT
Stichwörter:Saturnian Satellites, Icy satellites, Mimas, Tethys, Dione, Rhea, Iapetus, Phoebe, Hyperion
HGF - Forschungsbereich:Verkehr und Weltraum (alt)
HGF - Programm:Weltraum (alt)
HGF - Programmthema:W EW - Erforschung des Weltraums
DLR - Schwerpunkt:Weltraum
DLR - Forschungsgebiet:W EW - Erforschung des Weltraums
DLR - Teilgebiet (Projekt, Vorhaben):W - Vorhaben CASSINI (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung
Hinterlegt von: Pieth, Susanne
Hinterlegt am:09 Dez 2009 14:43
Letzte Änderung:09 Dez 2009 14:43

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