|Numerical Scheme to Solve 3D Structure of Rotationally
Supported Gas Disks
|444, 5th International Conference of Numerical Modeling of Space Plasma Flows (ASTRONUM 2010)
|Hanawa, T.; Kikuchi, D.; Otomo, Y.
|We propose two methods to improve numerical simulations of
rotating gas disks. One of them is introduction of the
reference velocity and the other is the velocity gradient
within a numerical cell. Both of them evaluate the centrifugal
force with better accuracy. These are applied to a young
accreting binary, a protoplanetary disk with a planet, and
a galactic gas disk. The numerical examples as well as the
methods are shown. The application to the galactic disk
suggests us the possibility that the wiggle instability
is likely to be of numerical origin.