Vertical Structure of a Magnetic Accretion Disk

Abstract

The vertical equation of a magnetic disk is solved on the approximation that the disk is geometrically thin, and its whole structure is investigated. The solutions are obtained in the form that we can apply them not only to an accretion flow, but also to a stellar wind. The disk is determined by the values of a thickness parameter of the disk 8 ( 1) of the corotation radius rc to the Alfven one ra. It is found that the magnetic disk consisting of a perfectly conductive plasma can exist in the super-Alfvenic region given by 8 3 r S'3 1+ (2S'3-1)5!2 ra), even if 8 1) in order to obtain stable magnetic disks in the super-Alfvenic region.