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-symmetric radiative wind model in which the relative contribution of thin lines increases from pole to equator. The introduction of a viscosity parameter enables us to consider the effects of a viscous force in the azimuthal component of momentum equations, The model gives hydrogen density law and velocity fields (v(r)(r,theta) and v(phi)(r,theta)) having assumed a temperature distribution. The ionization-excitation equilibrium is computed within the Sobolev approximation. The line profiles derived indicate that asymmetric double-peaked emission lines results from an expanding and rotating wind. The widths at half maximum of our profiles however are too large due to the strongly accelerated radial 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 alpha 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.