(Received April 26, 1978)
The structure of a stationary accretion disk surrounding a black hole is studied numerically under various outer boundary conditions. Numerical results indicate that the structure of the stationary accretion disk depends sensitively on the outer boundary condition. It is shown that current thin accretion disk models hold only for the extremely limited range of the outer boundary condition. For the other range of outer boundary condition, as we solve equations inwards, a rapid increase (or decrease) in the surface density begins at the far distance from the black hole. In the case of an optically thick accretion disk we have failed to find any solution which extends to the vicinity of the black hole. In the case of an optically thin accretion disk we can determine the whole structure, if we adopt an appropriate outer boundary condition. However, the feature of this solution differs substantially from current thin accretion disk models.
URL : http://ptp.ipap.jp/link?PTP/60/985/
DOI : 10.1143/PTP.60.985