N-body Simulations of Planetary Accretion around M Dwarf Stars

Details N-body Simulations of Planetary Accretion around M Dwarf Stars N-body Simulations of Planetary Accretion around M Dwarf Stars

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1158..259o&link_type=abstract

EXOPLANETS AND DISKS: THEIR FORMATION AND DIVERSITY: Proceedings of the International Conference. AIP Conference Proceedings, V

Physics

Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae, Accretion And Accretion Disks, Ground-Based Ultraviolet, Optical And Infrared Telescopes, General, Solar Nebula, Cosmogony

Scientific paper

We have investigated planetary accretion from planetesimals in terrestrial planet regions around M dwarf stars through N-body simulations including tidal interactions with disk gas. Because of the low luminosity of M dwarfs, habitable zones (HZs) are located in inner regions. In the close-in region, type-I migration is efficient according to the high disk gas density, although there is a large uncertainty in migration speed. Through a series of N-body simulations, we found that the final orbital configurations of the close-in terrestrial planets sensitively depend on the strength of type-I migration.

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