LINE-PROFILES AND INTENSITY MAPS FROM AN AXISYMMETRICAL RADIATIVE WIND MODEL FOR BE STARS

We present theoretical line profiles and intensity maps from an axi-sy mmetric radiative wind model in which the relative contribution of thi n lines increases from pole to equator. The introduction of a viscosit y parameter enables us to consider the effects of a viscous force in t he azimuthal component of momentum equations, The model gives hydrogen density law and velocity fields (v(r)(r,theta) and v(phi)(r,theta)) h aving assumed a temperature distribution. The ionization-excitation eq uilibrium is computed within the Sobolev approximation. The line profi les derived indicate that asymmetric double-peaked emission lines resu lts from an expanding and rotating wind. The widths at half maximum of our profiles however are too large due to the strongly accelerated ra dial flow present in the equatorial region. On the other hand they may provide an alternative explanation for the extended wings observed in some Be stars. The intensity maps show different morphologies in H al pha and H beta bands. With the advent of new interferometric data the comparison of intensity maps with high angular measurements may be an important test for Be star models.