Planetary Migration in non-isothermal disks

Details Planetary Migration in non-isothermal disks Planetary Migration in non-isothermal disks

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5811c&link_type=abstract

American Astronomical Society, DPS meeting #40, #58.11; Bulletin of the American Astronomical Society, Vol. 40, p.504

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Scientific paper

The torque felt by a planet orbiting in a radiatively inefficient gas disks has been studied by Paardekooper and Mellema (2006, 2008), Baruteau and Masset (2008), as well as by Paardekooper and Papaloizou (2008). In non locally isothermal disks, a positive corotation torque appears. This torque acts against the negative differential Lindblad torque, responsible for the well-known type I migration, directed inwards. However, with an adiabatic equation of state, the corotation torque saturates and vanishes.
Kley and Crida (2008) have shown that, with an energy equation including viscous heating, thermal diffusion, and radiative cooling from the surface of the disk, the total torque felt by a 20 Earth mass planet converges to a positive value. They found outward migration for planets of masses less than 40 Earth masses, while the migration regime appears to be almost independent of the energy equation for planets larger than 80 Earth masses.
This result will be presented, with possible extensions towards a better understanding of the migration rate as a function of the planet mass, the opacity law, and the disk parameters.
This behavior has strong implications for planetary evolution models. Consequences on the early dynamics of the outer Solar System will be shown.

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