Orbital Migration and Disc--Planet Interactions

Details Orbital Migration and Disc--Planet Interactions Orbital Migration and Disc--Planet Interactions

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..321..367n&link_type=abstract

Extrasolar Planets: Today and Tomorrow, ASP Conference Proceedings, Vol. 321, held 30 June - 4 July 2003, Institut D'Astrophysiq

Astronomy and Astrophysics

Astrophysics

8

Scientific paper

In this article we present a brief review of recent work on the interaction between protostellar discs and protoplanets. We describe in greater detail the results of recent simulations which examine the evolution of planets in magnetised, turbulent, protostellar discs. We review the similarities and differences between these simulations and laminar, viscous disc models. The main results are: high mass planets form gaps and migrate inward at the expected type II migration rate; massive planets can modify the turbulence and magnetic stresses locally within the gap region; magnetic linkage between the protostellar disc and circumplanetary disc causes magnetic braking of the latter, affecting the accretion rates onto giant planets; turbulent density fluctuations cause low mass protoplanets to undergo stochastic migration, which may modify the usual type I migration picture.

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