3D MHD simulations of planet migration in turbulent stratified disks

Details 3D MHD simulations of planet migration in turbulent stratified disks 3D MHD simulations of planet migration in turbulent stratified disks

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..276..515u&link_type=abstract

The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution, Proceedings of the International Astronomi

Astronomy and Astrophysics

Astrophysics

Accretion Disks, Mhd, Turbulence, Planetary Systems: Formation

Scientific paper

We performed 3D MHD numerical simulations of planet migration in stratified disks using the Godunov code PLUTO (Mignone et al. 2007). The disk is invaded by turbulence generated by the magnetorotational instability (MRI). We study the migration for planets with different mass to primary mass ratio. The migration of the low-mass planet (q=Mp/Ms=10-5) is dominated by random fluctuations in the torque and there is no defined direction of migration on timescales of 100 orbits. The intermediate-mass planet (q=Mp/Ms=10-4) can experience systematic outwards migration that was sustained for the times we were able to simulate.

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