Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 370, Issue 2, Pages 784-798Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2006.10506.x
Keywords
accretion, accretion discs; hydrodynamics; planets and satellites : general; galaxies : kinematics and dynamics
Categories
Ask authors/readers for more resources
The migration of a planet through a gaseous disc causes the locations of their resonant interactions to drift and can alter the torques exerted between the planet and the disc. We analyse the time-dependent dynamics of a non-coorbital corotation resonance under these circumstances. The ratio of the resonant torque in a steady state to the value given by Goldreich & Tremaine depends essentially on two dimensionless quantities: a dimensionless turbulent diffusion time-scale and a dimensionless radial drift speed. The dimensionless diffusion time-scale is a characteristic ratio of the time-scale of turbulent viscous diffusion across the librating region of the resonance to the time-scale of libration; in the absence of migration, this parameter alone determines the degree of saturation of the resonance. The dimensionless radial drift speed is the characteristic ratio of the drift speed of the resonance to the radial velocity in the librating region; this parameter determines the shape of the streamlines. When the drift speed is comparable to the libration speed and the viscosity is small, the torque can become much larger than the unsaturated value in the absence of migration, but is still proportional to the large-scale vortensity gradient in the disc. Fluid that is trapped in the resonance and drifts with it acquires a vortensity anomaly relative to its surroundings. If the anomaly is limited by viscous diffusion in a steady state, the resulting torque is inversely proportional to the viscosity, although a long time may be required to achieve this state. A further, viscosity-independent, contribution to the torque comes from fluid that streams through the resonant region. In other cases, torque oscillations occur before the steady value is achieved. We discuss the significance of these results for the evolution of eccentricity in protoplanetary systems. We also describe the possible application of these findings to the coorbital region and the concept of runaway (or type III) migration.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available