Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6305c&link_type=abstract
American Astronomical Society, DPS meeting #38, #63.05; Bulletin of the American Astronomical Society, Vol. 38, p.611
Astronomy and Astrophysics
Astronomy
Scientific paper
Planets exchange angular momentum with the protoplanetary nebula, and consequently they migrate and possibly open gaps in the disk.
Using a new algorithm in which the global evolution of the disk is modelled with combination of 1D and 2D grids (Crida et al, submitted to A&A), we computed a series of simulations of the evolution of Jupiter mass planets. For low viscosity, the migration occurs on a viscous timescale, as expected; however, when viscosity increases, the migration becomes slower, until it is cancelled or even reversed. This is because the gap is not completely gas-proof (so that the planet decouples from the gas evolution), and the corotation torque is positive and does not saturate (Masset 2001). This new result may provide a solution to the crucial problem of the planetary migration.
When a planet opens a gap, the inner disk is supposed to accrete on the central star, leading to the formation of a cavity. However, if the gap is gas-proof, the planet migrates inwards in the cavity opening timescale; if not, the inner disk does not empty completely. We observed that the density profile of the disk corresponds to the one described by the Lynden-Bell and Pringle (1974) equations, multiplied by the gap profile (fraction of the unperturbed density characterizing the equilibrium of the planet-disk interaction; Crida et al, 2006). The key parameter for cavity opening appears to be the ratio between the inner radius of the disk R_inf and the radius of the planetary orbit. The importance of R_inf had never been noticed before; it shows that the simulations need to account for the full extension of the gas disk, in particular down to its inner edge.
Crida Aurelien
Masset Frédéric
Morbidelli Alessandro
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