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Disk dynamics and planet migration

Published online by Cambridge University Press:  06 January 2010

T. Montmerle ,
D. Ehrenreich ,
A.-M. Lagrange  and
C. E.J.M.L.J. Terquem
C. E.J.M.L.J. Terquem*
Affiliation:
Institut d'Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie Paris 06, 98 bis Bd. Arago, 75014 Paris, France
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Abstract

We review models of protoplanetary disks. In the earlier stages of evolution, disks are subject to gravitational instabilities that redistribute mass and angular momentum on short timescales. Later on, when the mass of the disk is below ten percent or so of that of the central star, accretion occurs through the magnetorotational instability. The parts of the disks that are not ionized enough to couple to the magnetic field may not accrete or accrete inefficiently.
We also review theories of planet migration. Tidal interaction between a disk and an embedded planet leads to angular momentum exchange between the planetary orbital motion and the disk rotation. This results in low mass planets migrating with respect to the gas in the disk, while massive planets open up a gap in the vicinity of their orbit and migrate in as the disk is accreted.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 41: Physics and Astrophysics of Planetary Systems , 2010 , pp. 209 - 218
Copyright
© EAS, EDP Sciences, 2010

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