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Interior Evolution and Habitability

Spohn, T. und Breuer, D. (2007) Interior Evolution and Habitability. In: 2nd European Planetary Science Congress, . European Planetary Science Congress (EPSC), 2007-08-20 - 2007-08-24, Potsdam, Germany.

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Kurzfassung

Planetary habitability is usually thought to require water on (or near) the surface, a magnetic field to protect life against cosmic radiation, and transport mechanisms for nutrients. A magnetic field also serves to protect an existing atmosphere against erosion by the solar wind and thus helps to stabilize the presence of water and habitability. Magnetic fields are generated in the cores of the terrestrial planets and thus habitability is linked to the evolution of the interior. Moreover, the interior is a potential source as well as a sink for water and may interact with the surface reservoirs through volcanic activity and recycling. The simplest mechanism for recycling is plate tectonics. Plate tectonics is known to operate - at present - only on the Earth, although Mars may have had a phase of plate tectonics as may have Venus. Single-plate tectonics associated with stagnant lid convection – the present tectonic styles of the later planets - can also transfer water from the interior but a simple recycling mechanism is lacking. However, stagnant lid convection will evolve to thicken the lid and increasingly frustrate volcanic activity and degassing. This will keep the interior from running completely dry. Plate tectonics also facilitates generation of a magnetic field by effectively cooling the deep interior. For Mars and Venus it is likely that a present-day magnetic field would require plate tectonics to operate. An early field is possible even with stagnant lid convection but the dynamo will only operate less than 1 Ga under these circumstances. A question is then whether or not plate tectonics existed on Mars and Venus and if yes, why plate tectonics will cease to operate. Model calculations suggest elations to the yield strength of the mantle and the effect of water on the latter. Other models suggest at the existence of an asthenosphere (low viscosity zone underneath the lithosphere) is decisive and the dependence of its existence on the water content of the mantle.

Dokumentart:Konferenzbeitrag (Vortrag)
Titel:Interior Evolution and Habitability
Autoren:
AutorenInstitution oder E-Mail-Adresse der Autoren
Spohn, T.NICHT SPEZIFIZIERT
Breuer, D.NICHT SPEZIFIZIERT
Datum:August 2007
Erschienen in:2nd European Planetary Science Congress
Referierte Publikation:Nein
In SCOPUS:Nein
In ISI Web of Science:Nein
Seitenbereich:
Status:veröffentlicht
Stichwörter:Mars, habitability
Veranstaltungstitel:European Planetary Science Congress (EPSC)
Veranstaltungsort:Potsdam, Germany
Veranstaltungsart:internationale Konferenz
Veranstaltungsdatum:2007-08-20 - 2007-08-24
Veranstalter :Europlanet (European Planetology Network)
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: Stefanie Musiol
Hinterlegt am:29 Aug 2007
Letzte Änderung:27 Apr 2009 14:19

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