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Title:
The minimum gap-opening planet mass in an irradiated circumstellar accretion disc
Authors:
Edgar, Richard G.; Quillen, Alice C.; Park, Jaehong
Affiliation:
AA(Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA; ), AB(Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA; ), AC(Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA; )
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 381, Issue 3, pp. 1280-1286. (MNRAS Homepage)
Publication Date:
11/2007
Origin:
MNRAS
MNRAS Keywords:
accretian discs , planetary systems: protoplanetary discs
Abstract Copyright:
(c) 2007 The Authors. Journal compilation © 2007 RAS
DOI:
10.1111/j.1365-2966.2007.12305.x
Bibliographic Code:
2007MNRAS.381.1280E

Abstract

We consider the minimum mass planet, as a function of radius, that is capable of opening a gap in an α-accretion disc. We estimate that a half-Jupiter mass planet can open a gap in a disc with accretion rate for viscosity parameter α = 0.01, and solar mass and luminosity. The minimum mass is approximately proportional to . This estimate can be used to rule out the presence of massive planets in gapless accretion discs. We identify two radii at which an inwardly migrating planet may become able to open a gap and so slow its migration; the radius at which the heating from viscous dissipation is similar to that from stellar radiation in a flared disc, and the radius at which the disc becomes optically thin in a self-shadowed disc. In the inner portions of the disc, we find that the minimum planet mass required to open a gap is only weakly dependent on radius. If a migrating planet is unable to open a gap by the time it reaches either of the transition radii, then it is likely to be lost on to the star. If a gap-opening planet cuts off disc accretion allowing the formation of a central hole or clearing in the disc then we would estimate that the clearing radius would approximately be proportional to the stellar mass.
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