Wave Excitation in Accretion Disks by Protoplanets

Details Wave Excitation in Accretion Disks by Protoplanets Wave Excitation in Accretion Disks by Protoplanets

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.7107k&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #71.07; Bulletin of the American Astronomical Society, Vol. 34, p.761

Astronomy and Astrophysics

Astronomy

Scientific paper

The ongoing discoveries of extrasolar planets in the recent years revealed remarkable properties and unexpected results concerning the formation process. We studied the perturbation of a protostellar accretion disk by a companion utilizing APOLLO, a fast hydro disk code well tested in the case of accretion disks without a companion (Li et al. 2001, ApJ, 551, 874). We consider limiting cases where the companion's mass is much smaller than the central protostar and resides in a circular keplerian orbit. The gravitational field of the protoplanet, embedded in a numerically thin disk, generates spiral density waves and Rossby instabilities resulting in a non-axisymmetric density distribution. We present nonlinear hydro simulations to investigate those non-axisymmetric density distribution with different disk and planet parameters in order to understand how disks respond to a fixed companion in orbit. This work has been supported by IGPP at LANL (award # 1109) and NASA (grant # NAG5-9223).

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