Corotation torques experienced by planets embedded in weakly magnetized turbulent discs
Por:
Baruteau C., Fromang S., Nelson R.P., Masset F.
Publicada:
1 sep 2011
Resumen:
Context. The migration of low-mass planets, or type I migration, is driven by the differential Lindblad torque and the corotation torque in non-magnetic viscous models of protoplanetary discs. The corotation torque has recently received detailed attention, because of its ability to slow down, stall, or reverse type I migration. In laminar viscous disc models, the long-term evolution of the corotation torque is intimately related to viscous and thermal diffusion processes in the planet's horseshoe region. It is unclear how the corotation torque behaves in turbulent discs, and whether its amplitude is correctly predicted by viscous disc models. Aims. This paper is aimed at examining the properties of the corotation torque in discs where magnetohydrodynamic (MHD) turbulence develops as a result of the magnetorotational instability (MRI), considering a weak initial toroidal magnetic field. Methods. We present results of 3D MHD simulations carried out with two different codes. Non-ideal MHD
Filiaciones:
Baruteau C.:
DAMTP, University of Cambridge, Wilberforce Road, Cambridge CB30, WA, United Kingdom
Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, United States
Fromang S.:
Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/SAp, 91191 Gif-sur-Yvette, France
Nelson R.P.:
Astronomy Unit, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom
Masset F.:
Univ Nacl Autonoma Mexico, Inst Ciencias Fis, Cuernavaca 62251, Morelos, Mexico
Bronze
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