3D Simulations of Planet Migration
Contact: A. Uribe
Understanding planet migration is fundamental in explaining and predicting the distribution of observed exoplanets through planet population synthesis models and in testing planet formation theories against observations. Current analytical estimates of planet migration rates suggest very short migration times in comparison with disk lifetime timescales. Simulations of planet-disk interactions have confirmed these estimates and current work focuses on adding more relevant physical elements to the picture. Since protoplanetary disks are believed to be turbulent, there is great interest in studying planet migration in magnetized turbulent disks where the turbulence is generated by the magneto-rotational instability (MRI).
In my thesis project I intend to study planet migration rates and general planet-disk interaction (flow around the planet, gap opening, magnetic field structure) in magnetized turbulent disks, using 3D HD and MHD simulations, taking into account the planet's gas accretion and the vertical stratification of the disk.
Logarithm of the gas density from an MHD simulation of a Jupiter-mass planet embedded in a turbulent protoplanetary disk. The disk extends from 1 to 10 AU, and the planet is located at 3.3 AU.
