EDP Sciences
Free Access
Volume 459, Number 1, November III 2006
Page(s) L17 - L20
Section Letters
DOI https://doi.org/10.1051/0004-6361:20066304
Published online 27 September 2006

A&A 459, L17-L20 (2006)
DOI: 10.1051/0004-6361:20066304


Halting type I planet migration in non-isothermal disks

S.-J. Paardekooper1 and G. Mellema2, 1

1  Leiden Observatory, Postbus 9513, 2300 RA Leiden, The Netherlands
    e-mail: paardeko@strw.leidenuniv.nl
2  Stockholm Observatory, AlbaNova University Center, Stockholm University, 106 91 Stockholm, Sweden
    e-mail: garrelt@astro.su.se

(Received 28 August 2006 / Accepted 20 September 2006)

Aims.We investigate the effect of including a proper energy balance on the interaction of a low-mass planet with a protoplanetary disk.
Methods.We use a three-dimensional version of the RODEO method to perform hydrodynamical simulations including the energy equation. Radiation is included in the flux-limited diffusion approach.
Results.The sign of the torque is sensitive to the ability of the disk to radiate away the energy generated in the immediate surroundings of the planet. In the case of high opacity, corresponding to the dense inner regions of protoplanetary disks, migration is directed outward, instead of the usual inward migration that was found in locally isothermal disks. For low values of the opacity we recover inward migration and show that torques originating in the coorbital region are responsible for the change in migration direction.

Key words: radiative transfer -- hydrodynamics -- methods: numerical -- planets and satellites: formation

© ESO 2006

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