We have examined the radial structure of the outer region of self-gravitation and magnetized accretion disk, which is closely related to the line and continuum emission from the outer region of the disk. We have adopted the different opacities in different regime as the work by SCD (1990II). Our some results are very similar to SCD's, such as in regimes A, C, E, , , and decrease with increasing radii of different functions. In regimes D and F, are constant, and , decrease with increasing radii of different functions. In addition, the profiles of our figures are also very similar to CSD's(1990II) figures. But our results have some differences from CSD's work (1990II). That is: the first is that our is greater than . ( is the same as
CSD's , 1990II), so our may be important to the line formation (next paper we are going to disscuse its effect on the line forming).The second is the line formation region extents to the outer region because our is bigger than CSD's( 1990II) about 1.54 times. The third is that our is much thinner than CSD's(1990II). All these differences come from the effects of self-gravitation and magnetic field.
© European Southern Observatory (ESO) 1997
Online publication: April 8, 1998