Line Profiles Dependent on the Opacity Parameter in AZ CAS

Abstract

The binary system AZ Cas consists of a main sequence star of B type and a late type and a late type supergaint with extended atmospheric. In other to present the effect of mass flow from the supergaint which fills its Roche lobe, line profiles were calculated at phaces 0.05 and 0.09 under different assumptions regarding the opacity parameter. Hempe's sobolev method(1982) for the source function was used in this paper. For the higher opacity parameter, the line profiles are shown to be stronger due to the higher number densities of absorbers. At phase 0.05, the line profiles have bumps at red end of absorption part, which can be explained by the reemission superimposed on the lline profile of absorption part.