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Geophysical and Atmospheric Evolution of Habitable Planets

H. Lammer ; F. Selsis ; E. Chassefière ; D. Breuer ; J.-M. Grießmeier ; Y. N. Kulikov ; N. V. Erkaev ; M. L. Khodachenko ; H. K. Biernat ; F. Leblanc ; E. Kallio ; R. Lundin ; F. Westall ; S. J. Bauer ; C. Beichman ; W. Danchi ; C. Eiroa ; M. Fridlund ; H. Gröller ; A. Hanslmeier ; W. Hausleitner ; T. Henning ; T. Herbst ; L. Kaltenegger ; A. Léger ; M. Leitzinger ; H. I. M. Lichtenegger ; René Liseau (Institutionen för radio- och rymdvetenskap, Radioastronomi och astrofysik) ; J. Lunine ; U. Motschmann ; P. Odert ; F. Paresce ; J. Parnell ; A. Penny ; A. Quirrenbach ; H. Rauer ; H. Röttgering ; J. Schneider ; T. Spohn ; A. Stadelmann ; G. Stangl ; D. Stam ; G. Tinetti ; G. J. White
Astrobiology (1531-1074). Vol. 10 (2010), 1, p. 45-68.
[Artikel, refereegranskad vetenskaplig]

The evolution of Earth-like habitable planets is a complex process that depends on the geodynamical and geophysical environments. In particular, it is necessary that plate tectonics remain active over billions of years. These geophysically active environments are strongly coupled to a planet's host star parameters, such as mass, luminosity and activity, orbit location of the habitable zone, and the planet's initial water inventory. Depending on the host star's radiation and particle flux evolution, the composition in the thermosphere, and the availability of an active magnetic dynamo, the atmospheres of Earth-like planets within their habitable zones are differently affected due to thermal and nonthermal escape processes. For some planets, strong atmospheric escape could even effect the stability of the atmosphere.



Denna post skapades 2010-12-20. Senast ändrad 2010-12-21.
CPL Pubid: 131361

 

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Institutioner (Chalmers)

Institutionen för radio- och rymdvetenskap, Radioastronomi och astrofysik (2005-2010)

Ämnesområden

Astronomi
Planetsystemet

Chalmers infrastruktur