The core accretion model predicts few Jovian-mass planets orbiting red dwarfs

被引:343
作者
Laughlin, G [1 ]
Bodenheimer, P
Adams, FC
机构
[1] Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA
[2] Univ Michigan, Dept Phys, Michigan Ctr Theoret Phys, Randall Lab 2477, Ann Arbor, MI 48109 USA
[3] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA
基金
美国国家航空航天局;
关键词
planetary systems : formation; planetary systems : protoplanetary disks; stars : formation;
D O I
10.1086/424384
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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.
引用
收藏
页码:L73 / L76
页数:4
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