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Formation of terrestrial planets from planetesimals around M dwarfs

Published online by Cambridge University Press:  01 October 2007

Masahiro Ogihara  and
Shigeru Ida
Masahiro Ogihara
Affiliation:
Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1-I2-10 Ookayama, Meguro-ku, Tokyo 152-8551, Japan email: ogihara@geo.titech.ac.jp, ida@geo.titech.ac.jp
Shigeru Ida
Affiliation:
Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1-I2-10 Ookayama, Meguro-ku, Tokyo 152-8551, Japan email: ogihara@geo.titech.ac.jp, ida@geo.titech.ac.jp
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Abstract

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We have investigated accretion of terrestrial planets from planetesimals around M dwarfs through N-body simulations including the effect of tidal interaction with disk gas. Because of low luminosity of M dwarfs, habitable zones around them are located near the disk inner edge. Planetary embryos undergo type-I migration and pile up near the disk inner edge. We found that after repeated close scatterings and occasional collisions, three or four planets eventually remain in stable orbits in their mean motion resonances. Furthermore, large amount of water-rich planetesimals rapidly migrate to the terrestrial planet regions from outside of the snow line, so that formed planets in these regions have much more water contents than those around solar-type stars.

Keywords

accretionaccretion disksmethods: n-body simulationsplanetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 305 - 308
Copyright
Copyright © International Astronomical Union 2008

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