Coupling 1D and 2D grids to compute global evolution of protoplanetary disks with embedded planets

Details Coupling 1D and 2D grids to compute global evolution of protoplanetary disks with embedded planets Coupling 1D and 2D grids to compute global evolution of protoplanetary disks with embedded planets

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sf2a.conf..747c&link_type=abstract

SF2A-2005: Semaine de l'Astrophysique Francaise, meeting held in Strasbourg, France, June 27 - July 1, 2005, Edited by F. Casoli

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Scientific paper

During planet formation, the protoplanets interact with the protoplanetary gas disk, leading to very interesting phenomena, like planetary migration. Numerical simulations are a precious tool for the study of these complex interactions. Typically, planet-disk interactions are computed using a 2D polar grid which, for numerical reasons, is truncated at an inner and an outer edge. This enables us to describe the local interaction of the planet with the disk but not the global evolution of the disk. Unfortunately though, the global viscous evolution of the disk governs type II migration (e.g. Ward 2003).
In order to model correctly the global evolution of the disk and the local planet-disk interaction, we have developed an improved version of F. Masset's FARGO hydrodynamical code. Outside of the boundaries of the 2D grid, we model the disk with two 1D grids. The first one extends from the surface of the star up to the inner edge of the 2D grid, and the other ranges from the outer border of the 2D grid up to an arbitrary large distance. The coupling between the 1D and 2D representations of the disk is done through the interfaces between the grids.

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