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Planet Migration in Nearly Laminar Disks

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If you have a question about this talk, please contact Dr Geoffroy Lesur.

Planet migration occurs as a young proto-planet moves radially through a gaseous disk. A problem is that the migration is inward and the timescales are generally found to be too short for planet formation in the standard core accretion model. Several mechanisms have been proposed to slow the planet migration. One mechanism involves slowing migration by a feedback effect that is predicted to occur if the disk turbulent viscosity is low. I describe recent results of nonlinear simulations of planet migration in a nearly laminar disk.

This talk is part of the DAMTP Astrophysics Seminars series.

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