DLR-Logo -> http://www.dlr.de
DLR Portal Home | Impressum | Kontakt | English
Schriftgröße: [-] Text [+]

Comparison of the Jovian and Saturnian satellites

Sohl, F. (2009) Comparison of the Jovian and Saturnian satellites. European Space Agency (ESA-ESTEC), Research and Scientific Support Department (RSSD) Open Seminar , 2009-12-11, Noordwijk, the Netherlands.

Dieses Archiv kann nicht den gesamten Text zur Verfügung stellen.


The understanding of outer planet satellites has improved considerably, when the Voyager spacecraft flew by Jupiter, Saturn, Uranus, and Neptune, followed by the advent of the Galileo spacecraft in the Jovian system (1995-2003) and the Cassini spacecraft in the Saturnian system (since 2004). We will be discussing geophysical constraints on the interior structure and composition of selected Jovian and Saturnian icy satellites and investigate conditions under which potentially habitable liquid water reservoirs could be maintained. Active volcanism on Io and tectonic features on Europa emphasize the importance of tidal heating in the Jupiter system, maintained by gravitational interaction due to the resonant orbits of Io, Europa, and Ganymede (Laplace resonance). Ganymede is strongly differentiated and possesses a self-sustained, dipolar magnetic field. Magnetic induction signals were observed at Europa, Callisto, and possibly Ganymede, suggesting the presence of globe-encircling, briny reservoirs of liquid water below the surface. Saturn's largest moon Titan is intermediate between Ganymede and Callisto in respect to its radius, mean density and degree of internal differentiation. Titan is likely to harbour a cold, extended internal liquid reservoir, similar to the large icy satellites of Jupiter, but more enriched in ammonia. Enceladus' south pole hot spot and associated water-vapour plumes may be caused by localized tidal heating above a liquid water reservoir in contact with silicate rock below. Interior models of icy bodies would certainly benefit from future geophysical exploration, which would include gravitational and magnetic field sounding from low-altitude orbit and close flyby, combined with altimetry data and in-situ monitoring of tidally-induced surface distortion and time-variable magnetic fields. Additional important constraints are provided by the surface geology, spectral properties, and chemistry of each individual satellite.

Dokumentart:Konferenzbeitrag (Vorlesung)
Titel:Comparison of the Jovian and Saturnian satellites
AutorenInstitution oder E-Mail-AdresseAutoren-ORCID
Datum:Dezember 2009
In Open Access:Nein
In ISI Web of Science:Nein
Stichwörter:Outer planet satellites, interiors, surfaces, tides, water oceans, Io, Europa, Ganymede, Callisto, Enceladus, Titan
Veranstaltungstitel:European Space Agency (ESA-ESTEC), Research and Scientific Support Department (RSSD) Open Seminar
Veranstaltungsort:Noordwijk, the Netherlands
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 Vergleichende Planetologie (alt)
Standort: Berlin-Adlershof
Institute & Einrichtungen:Institut für Planetenforschung > Planetenphysik
Hinterlegt von: Sohl, Frank
Hinterlegt am:05 Jan 2010 13:41
Letzte Änderung:05 Jan 2010 13:41

Nur für Mitarbeiter des Archivs: Kontrollseite des Eintrags

Hilfe & Kontakt
electronic library verwendet EPrints 3.3.12
Copyright © 2008-2017 Deutsches Zentrum für Luft- und Raumfahrt (DLR). Alle Rechte vorbehalten.