HR: 1340h
AN: SA53B-1182 [Abstracts]
TI: The Kelvin-Helmholtz instability induced by the Magneto-rotational instability in the inner-edge region
of an accretion disk ; MHD simulations with CIP-MOCCT method
AU: * Nakamura, K
EM: knakamur@geo.titech.ac.jp
AF: Department of Earth and Planetary Sciences
Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo, 152-8551
Japan
AU: Tandokoro, R
EM: rtdokoro@geo.titech.ac.jp
AF: Department of Earth and Planetary Sciences
Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo, 152-8551
Japan
AU: Fujimoto, M
EM: fujimoto@geo.titech.ac.jp
AF: Department of Earth and Planetary Sciences
Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo, 152-8551
Japan
AU: Ida, S
EM: ida@geo.titech.ac.jp
AF: Department of Earth and Planetary Sciences
Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo, 152-8551
Japan
AB:
Around protostars, the gases and the dusts falling to these objects form the rotating disks called accretion disks. When an
accretion disk has a weak magnetic field, it is well known that the magneto-rotational instability (MRI) is excited in the
disks. By using the local 2.5-dimensional MHD simulations with CIP-MOCCT method, we confirmed the generation of MRI and
investigated the influences of MRI on the disks in accretion disks. Especially, we have done modeling of the boundary region
(inner-edge) between the magnetosphere of a central star and an accretion disk. In this case the disk part is disturbed by
MRI while the magnetospheric strong magnetic field does not allow MRI effects to propagate into the magnetosphere. Then large
velocity shear is generated at the inner-edge. This result implies that the Kelvin-Helmholtz instability might be excited at
the inner-edge. Actually, performing a 3-dimensional simulation, we observe the Kelvin-Helmholtz instability to be excited
at the inner-edge. Implication of this result to the planetary system formation processes is discussed.
DE: 6030 Magnetic fields and magnetism
DE: 6050 Plasma and MHD instabilities (2149, 2752, 7836)
DE: 7524 Magnetic fields
DE: 7836 MHD waves and instabilities (2149, 2752, 6050)
DE: 7863 Turbulence (4490)
SC: SPA-Aeronomy [SA]
MN: Fall Meeting 2005