TY - JOUR
T1 - Numerical simulations of two-dimensional and three-dimensional accretion flows
AU - Matsuda, Takuya
AU - Ishii, Takanori
AU - Sekino, Nobuhiro
AU - Sawada, Keisuke
AU - Shima, Eiji
AU - Livio, Mario
AU - Anzer, Ulrich
N1 - Funding Information:
The present calculations were performed on the Fujitsu VP400E at the Data Processing Center of Kyoto University, the VP400E and Hitachi S820 at the Institute of Computational Fluid Dynamics, Tokyo, and the VP400E at the Kan-sai Institute of Computational Fluid Dynamics, Osaka. The Japanese authors would like to thank Professor K. Kuwahara for his help. TM was supported by the Grant-in-Aid for Scientific Research (01540221, 02234206) of the Ministry of Education, Science and Culture in Japan.
Publisher Copyright:
© 1992 Oxford University Press. All rights reserved.
PY - 1992
Y1 - 1992
N2 - Numerical simulations of 2D and 3D accretion flows past a gravitating compact object from a uniform flow at a large distance upstream are performed by solving the Eulerian equations. We find that 2D flows exhibit a 'flip-flop instability' if the central accreting body is small. If the central body is enlarged at some instance in the oscillating flow, then the accretion shock shows a rather periodic oscillation similar to the von Karman vortex street. In the case of 3D flows, it is found that the shock cone is much more robust than in 2D, and the flip-flop instability takes a different, probably less violent form. The causes for the instabilities are discussed.
AB - Numerical simulations of 2D and 3D accretion flows past a gravitating compact object from a uniform flow at a large distance upstream are performed by solving the Eulerian equations. We find that 2D flows exhibit a 'flip-flop instability' if the central accreting body is small. If the central body is enlarged at some instance in the oscillating flow, then the accretion shock shows a rather periodic oscillation similar to the von Karman vortex street. In the case of 3D flows, it is found that the shock cone is much more robust than in 2D, and the flip-flop instability takes a different, probably less violent form. The causes for the instabilities are discussed.
UR - http://www.scopus.com/inward/record.url?scp=0000003990&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=0000003990&partnerID=8YFLogxK
U2 - 10.1093/mnras/255.2.183
DO - 10.1093/mnras/255.2.183
M3 - Article
AN - SCOPUS:0000003990
VL - 255
SP - 183
EP - 191
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -