Influences on planetary migration in 3D fully radiative discs

Details Influences on planetary migration in 3D fully radiative discs Influences on planetary migration in 3D fully radiative discs

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf..752b&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.752

Physics

Scientific paper

The inclusion of radiation transport in discs can change the direction of migration for low mass planets from inwards to outwards [1]. However, it remained unclear to what extend this outward migration is possible. Outward migration should stop at a certain distance to the central star. This region in the disc can therefore act as a feeding zone for planetary embryos. The magnitude of outward migration is also dependent on disc parameters (mass, viscosity, temperature profile, entropy gradient). A change in these parameters changes the disc structure and therefore the range of outward migration of embedded planets.

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