The equatorial plane of Be stars: an outflow driven by optically thin lines?

Details The equatorial plane of Be stars: an outflow driven by optically thin lines? The equatorial plane of Be stars: an outflow driven by optically thin lines?

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...298..179d&link_type=abstract

Astronomy and Astrophysics, v.298, p.179

Astronomy and Astrophysics

Astrophysics

6

Stars: Be, Circumstellar Matter, Stars: Mass-Loss, Hydrodynamics

Scientific paper

Accurate numerical solutions for the radial motion equation in the equatorial plane of rotating B-type stars are presented. We have considered an outflow driven mainly (or uniquely!) by optically thin lines. This is done by decreasing the value of the radiative parameter α in the domain (0.5>=α>=0.0). It was obtained a net shallowing of expansion with lower values of α. This conclusion seems independent of several assumptions as stellar rotation rate, temperature of the envelope, boundary condition. On the other hand reasonable mass fluxes require large values for the radiative parameter k. Our results give support to the idea that the dynamics in the equatorial region of Be star envelopes is dominated by a radiative force due to a great number of thin lines.

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