34th Meeting of the AAS Division on Dynamical Astronomy, May 2003
6 Poster Papers
Posters, Monday, May 5, 2003, 8:00pm,

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[6.08] Three-Dimensional Simulations of High and Low-Mass Planets Embedded in Protoplanetary Disks

S.H. Lubow (STScI), M.R. Bate (Univ of Exeter), G.I. Ogilvie (IoA), K.A. Miller (Univ of Maryland)

We analyze the non-linear, three-dimensional response of a gaseous, viscous protoplanetary disk to the presence of a planet of mass ranging from one Earth mass to one Jupiter mass by using the ZEUS hydrodynamics code. We determine the gas flow pattern, and the accretion and migration rates of the planet. The planet is assumed to be in a fixed circular orbit about the central star. It is also assumed to be able to accrete gas without expansion on the scale of its Roche radius. For typical parameters, only planets with masses greater than one-tenth Jupiter's mass produce significant perturbations in the disk's surface density. The flow within the Roche lobe of the planet is fully three-dimensional. Gas streams generally enter the Roche lobe close to the disk midplane, but produce much weaker shocks than the streams in two-dimensional models. The streams supply material to a circumplanetary disk that rotates in the same sense as the planet's orbit. Much of the mass supply to the circumplanetary disk comes from non-coplanar flow. The accretion rate peaks with a planet mass of approximately one-tenth Jupiter's mass and is highly efficient, occurring at the local viscous rate. The migration timescales for planets of mass less than one-tenth Jupiter's mass, based on torques from disk material outside the planets' Roche lobes, are in excellent agreement with the linear theory of Type I (non-gap) migration for three-dimensional disks. We find that it is difficult for planets to acquire as much as ten Jupiter masses before tidal forces cut off further accretion. We acknowledge support from NASA grant NAG5-10732.

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Bulletin of the American Astronomical Society, 35 #4
© 2003. The American Astronomical Soceity.