Institut für Astronomie & Astrophysik

Influence of the disc structure on planet migration

Bertram Bitsch

In isothermal protoplanetary discs around young stars, low mass planets (a few M_E) migrate inwards to the star on a very short timescale (type-I-migration). Infact, the timescale is so short that these planets would be lost inside the star before they could form bigger objects due to gas accretion (e.g. Jupiter-size planets). In recent years, however, the relaxation of the isothermal approach and the inclusion of viscous heating and radiative cooling resulted in a change of the migration rate. In certain cases the migration rate can even be reversed so that low mass planets (above a few M_E) can migrate outwards, which allows them to stay longer in the gas disc and eventually form gas giant planets. This migration reversal is caused by the so-called corotation torque and is strongly dependent on the gradients of temperature and entropy in the disc. I will explain the mechanism of the corotation torque that causes outward migration and show the limits of this outward migration in discs. I will then show the difference between flared and self-shaddowed discs and what that implies for the migration of planets.

Privacy settings

Our website uses cookies. Some of them are mandatory, while others allow us to improve your user experience on our website. The settings you have made can be edited at any time.

or

Essential

in2code

Videos

in2code
YouTube
Google