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2010MNRAS.408..876A - Mon. Not. R. Astron. Soc., 408, 876-896 (2010/October-3)
Planet migration: self-gravitating radiation hydrodynamical models of protoplanets with surfaces.
AYLIFFE B.A. and BATE M.R.
Abstract (from CDS):
These results are arrived at by calculating migration rates in locally isothermal models, before sequentially introducing self-gravity, and radiative transfer, allowing us to isolate the effects of the additional physics. We find that using a locally isothermal equation of state, without self-gravity, we reproduce the migration rates obtained by previous analytic and numerical models. We explore the impact of different protoplanet models, and changes to their assumed radii, upon migration. The introduction of self-gravity gives a slight reduction of the migration rates, whilst the inertial mass problem, which has been proposed for high-mass protoplanets with circumplanetary discs, is reproduced. Upon introducing radiative transfer to models of low-mass protoplanets (~10 M), modelled as small radius accreting point masses, we find outward migration with a rate of approximately twice the analytic inward rate. However, when modelling such a protoplanet in a more realistic manner, with a surface which enables the formation of a deep envelope, this outward migration is not seen.
Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS
Journal keyword(s): hydrodynamics - radiative transfer - methods: numerical - planets and satellites: formation - planet - disc interactions
Simbad objects: 1
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