Expanding envelopes of binary stars

In this paper which is a continuation of Neutsch and Schmidt (1985a) (later on referred to as part I) we shall investigate the structure of binary envelopes under the hypothesis that at least one of the companions produces a very intense radiation field. The limiting case in which the forces due to the system's rotation (i.e., Coriolis and centrifugal forces) as well as gas pressure can be neglected is solved analytically using a classical result of Euler. Beyond this the velocity and density distributions in the envelope are determined.Under the assumptions mentioned above, the results are exact and are, therefore, of value as a reference model for later more advanced considerations (see, e.g., Neutsch and Schmidt, 1985b). Although the present approach is quite simple, it nevertheless shows some typical features of the general case. Furthermore, it serves as a helpful guide in guessing the system parameters to be initially adopted in physically sounder. calculations (for example: the Monte-Carlo approximation which will be described in Part III).