Publikationsdatum:
2006-09-09
Beschreibung:
Close-in giant planets (e.g., "hot Jupiters") are thought to form far from their host stars and migrate inward, through the terrestrial planet zone, via torques with a massive gaseous disk. Here we simulate terrestrial planet growth during and after giant planet migration. Several-Earth-mass planets also form interior to the migrating jovian planet, analogous to recently discovered "hot Earths." Very-water-rich, Earth-mass planets form from surviving material outside the giant planet's orbit, often in the habitable zone and with low orbital eccentricities. More than a third of the known systems of giant planets may harbor Earth-like planets.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Raymond, Sean N -- Mandell, Avi M -- Sigurdsson, Steinn -- New York, N.Y. -- Science. 2006 Sep 8;313(5792):1413-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80309-0392, USA. raymond@lasp.colorado.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16960000" target="_blank"〉PubMed〈/a〉
Schlagwort(e):
Astronomical Phenomena
;
Astronomy
;
Computer Simulation
;
Earth (Planet)
;
*Evolution, Planetary
;
Iron
;
Mathematics
;
*Planets
;
Temperature
;
*Water
Print ISSN:
0036-8075
Digitale ISSN:
1095-9203
Thema:
Biologie
,
Chemie und Pharmazie
,
Informatik
,
Medizin
,
Allgemeine Naturwissenschaft
,
Physik
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