Numerical Simulations of Accretion Disks

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Session 32 -- Circumstellar Environments
Oral presentation, Wednesday, January 12, 2:15-3:45, Salon VI Room (Crystal Gateway)

[32.05] Numerical Simulations of Accretion Disks

R. Drimmel (University of Florida)

Two dimensional self-gravitating gaseous accretion disks are modeled using smoothed particle hydrodynamics, which allows a general solution to the hydrodynamical equations, in the sense that the disks are not forced to remain within a grid. An inner boundary condition allows for particles to naturally accret onto a central object. Such disks are representative of an early stage in the evolution of a solar system. The unstable non-axisymetric modes are found using Fourier techniques, and the nonlinear evolution of the modes followed. These modes redistribute the angular momentum, causing the disk to evolve. However, a second mechanism for redistributing the angular momentum is present in the shear viscocity, and its relative importance is discussed.

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