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The Core Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs

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Laughlin, Gregory, Bodenheimer, Peter, Adams, Fred C.·2004·The Astrophysical Journal

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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Metadata

Authors
Laughlin, G., Bodenheimer, P., & Adams, F. C.
Venue
The Astrophysical Journal
Published
2004-08-02
Volume
612
Issue
1
Pages
L73-L76
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2024770774
Cited by
440
References
0
FWCI
14.18
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: The Core Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs. https://app.cochat.ai/papers/10.1086/424384
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Laughlin, G., Bodenheimer, P., & Adams, F. C. (2004). The Core Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs. The Astrophysical Journal. https://doi.org/10.1086/424384

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