Numerical Simulations of Accretion Disks

Details Numerical Simulations of Accretion Disks Numerical Simulations of Accretion Disks

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.3205d&link_type=abstract

American Astronomical Society, 183rd AAS Meeting, #32.05; Bulletin of the American Astronomical Society, Vol. 25, p.1341

Astronomy and Astrophysics

Astronomy

Scientific paper

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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