paper

The interaction of planets with a disc with MHD turbulence IV: Migration rates of embedded protoplanets

arXiv:astro-ph/0308360 · doi:10.1111/j.1365-2966.2004.07406.x

Abstract

(Abridged) We present global disc and local shearing box simulations of planets interacting with a MHD turbulent disc. We examine the torque exerted by the disc on the embedded planets as a function of planet mass, and thus make a first study of orbital migration of planets due to interaction with turbulent discs. Global simulations were performed for a disc with H/R=0.07 and planet masses M_p=3,10,30 Earth masses, and 3 Jupiter masses. Shearing box runs were performed for values of (M_p/M_*)/(H/R)^3=0.1,0.3,1.0 and 2.0, M_* being the central mass. These allow embedded and gap forming planets to be examined. In all cases the instantaneous torque exerted on a planet showed strong fluctuations. In the embedded cases it oscillated between negative and positive values, and migration occurs as a random walk, unlike the usual type I migration. Running time averages for embedded planets over 20-25 orbital periods show that large fluctuations occur on longer time scales, preventing convergence of the average torque to well defined values, or even to a well defined sign. Fluctuations become relatively smaller for larger masses, giving better convergence, due to the planet's perturbation of the disc becoming larger than the turbulence in its vicinity. Eventually gap formation occurs, with a transition to type II migration. The existence of significant fluctuations occurring in turbulent discs on long time scales is important for lower mass embedded protoplanets. If significant fluctuations occur on the longest disc evolutionary time scales, convergence of torque running averages for practical purposes will not occur, and the migration behaviour of low mass protoplanets considered as an ensemble would be very different from predictions of type I theory for laminar discs.

19 pages, 24 figures (some colour), submitted to M.N.R.A.S. A gzipped postscript version containing high resolution colour figures is available from http://www.maths.qmul.ac.uk/~rpn

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