Line profiles and intensity maps from an axi-symmetric radiative wind model for Be stars

Details Line profiles and intensity maps from an axi-symmetric radiative wind model for Be stars Line profiles and intensity maps from an axi-symmetric radiative wind model for Be stars

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292..221s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 1, p. 221-238

Statistics

Computation

42

B Stars, Computational Astrophysics, Emission Spectra, Interstellar Matter, Magnetohydrodynamics, Stellar Mass, Stellar Models, Stellar Radiation, Stellar Winds, Angular Momentum, Approximation, Astronomical Maps, Equations Of Motion, H Alpha Line, H Beta Line, Radial Flow, Stellar Rotation

Scientific paper

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 (vr(r, theta) and vphi(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 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.

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