| Literature DB >> 20307182 |
Helmut Lammer1, Frank Selsis, Eric Chassefière, Doris Breuer, Jean-Mathias Griessmeier, Yuri N Kulikov, Nikolai V Erkaev, Maxim L Khodachenko, Helfried K Biernat, Francois Leblanc, Esa Kallio, Richard Lundin, Frances Westall, Siegfried J Bauer, Charles Beichman, William Danchi, Carlos Eiroa, Malcolm Fridlund, Hannes Gröller, Arnold Hanslmeier, Walter Hausleitner, Thomas Henning, Tom Herbst, Lisa Kaltenegger, Alain Léger, Martin Leitzinger, Herbert I M Lichtenegger, René Liseau, Jonathan Lunine, Uwe Motschmann, Petra Odert, Francesco Paresce, John Parnell, Alan Penny, Andreas Quirrenbach, Heike Rauer, Huub Röttgering, Jean Schneider, Tilman Spohn, Anja Stadelmann, Günter Stangl, Daphne Stam, Giovanna Tinetti, Glenn J White.
Abstract
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.Entities:
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Year: 2010 PMID： 20307182 DOI： 10.1089/ast.2009.0368
Source DB: PubMed Journal: Astrobiology ISSN： 1557-8070 Impact factor: 4.335