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Title:
The Core Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs
Authors:
Laughlin, Gregory; Bodenheimer, Peter; Adams, Fred C.
Affiliation:
AA(Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064 ), AB(Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064 ), AC(Michigan Center for Theoretical Physics, Department of Physics, University of Michigan, 2477 Randall Laboratory, 500 East University Avenue, Ann Arbor, MI 48109; Department of Astronomy, University of Michigan, 830 Dennison, 501 East University Avenue, Ann Arbor, MI 48109. )
Publication:
The Astrophysical Journal, Volume 612, Issue 1, pp. L73-L76. (ApJL Homepage)
Publication Date:
09/2004
Origin:
UCP
Astronomy Keywords:
Stars: Planetary Systems: Formation, Stars: Planetary Systems: Protoplanetary Disks, Stars: Formation
DOI:
10.1086/424384
Bibliographic Code:
2004ApJ...612L..73L

Abstract

The favored theoretical explanation for giant planet formation-in both our solar system and others-is the core accretion model (although it still has some serious difficulties). In this scenario, planetesimals accumulate to build up planetary cores, which then accrete nebular gas. With current opacity estimates for protoplanetary envelopes, this model predicts the formation of Jupiter-mass planets in 2-3 Myr at 5 AU around solar-mass stars, provided that the surface density of solids is enhanced over that of the minimum-mass solar nebula (by a factor of a few). Working within the core accretion paradigm, this Letter presents theoretical calculations that show that the formation of Jupiter-mass planets orbiting M dwarf stars is seriously inhibited at all radial locations (in sharp contrast to solar-type stars). Planet detection programs sensitive to companions of M dwarfs will test this prediction in the near future.
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