Building giant-planet cores at a planet trap
Por:
Morbidelli A., Crida A., Masset F., Nelson R.P.
Publicada:
1 feb 2008
Resumen:
Context. A well-known bottleneck for the core-accretion model of giant-planet formation is the loss of the cores into the star by type I migration, due to the tidal interactions with the gas disk. It has been shown that a steep surface-density gradient in the disk, such as the one expected at the boundary between an active and a dead zone, acts as a planet trap and prevents isolated cores from migrating down to the central star. Aims. We study the relevance of the planet trap concept for the accretion and evolution of systems of multiple planetary embryos/cores. Methods. We performed hydrodynamical simulations of the evolution of systems of multiple massive objects in the vicinity of a planet trap. The planetary embryos evolve in 3 dimensions, whereas the disk is modeled with a 2D grid. Synthetic forces are applied onto the embryos to mimic the damping effect that the disk has on their inclinations. Results. Systems with two embryos tend to acquire stable, separated and non-migrating o
Filiaciones:
Morbidelli A.:
Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France
Crida A.:
Institut für Astronomie and Astrophysik, Univ. of Tubingen, Germany
Masset F.:
Univ Nacl Autonoma Mexico, IA, Mexico City, DF, Mexico
Nelson R.P.:
Queen Mary, University of London, United Kingdom
Bronze
|