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G. Lufkin, T. Quinn, F. Governato (University of Washington)
We present fully self-consistent 3D Smoothed-Particle Hydrodynamics simulations of an isothermal gaseous circumstellar disk interacting with an embedded protoplanet. We calculate planet migration and accretion rates as a function of initial disk and planet masses. The rates are higher than previous analytic and numerical work has found, and we explore the discrepancy resulting from self-gravity, the vertical dimension, and adaptive spatial resolution. Under certain initial conditions the embedded planet can trigger gravitational instabilities, leading to further planet formation that would not occur in the absence of the first planet. Visualizations of each scenario are presented.
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Bulletin of the American Astronomical Society, 35 #4
© 2003. The American Astronomical Soceity.