Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5810w&link_type=abstract
American Astronomical Society, DPS meeting #40, #58.10; Bulletin of the American Astronomical Society, Vol. 40, p.504
Astronomy and Astrophysics
Astronomy
Scientific paper
Planet migration due to torques from the coorbital, corotation region of the solar nebula is examined. A simple 2D streamline modal is developed to elucidate the migration mechanism. The model is then modified to take into account effects that depend on the relative size of the horseshoe zone half-width, w, and nebula vertical scale height, h. This type III migration has a small planet regime where the rate increases steeply with the planet's mass until the horseshoe zone half-width becomes comparable to the disk scale height, w h. At this point there is an intermediate mass range where the migration is fast but mass insensitive, until the horseshoe zone width gets too wide for the planet to drift a distance w in a single horseshoe orbit libration period. For still higher masses, a slow regime appears where the migration rate decreases with mass until it eventually converges on the type I migration rate. However, the intermediate mass range only exists for sufficiently massive disks. When present, the type III migration rate generally exceeds that of type I migration by over an order of magnitude.
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