Volume 437, Number 3, July III 2005
|Page(s)||929 - 933|
|Section||Interstellar and circumstellar matter|
|Published online||30 June 2005|
Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
Departamento de Física y Meteorología, Facultad de Ciencias, Universidad de Valparaíso, Valparaíso, Chile e-mail: email@example.com
2 Departamento de Matemáticas, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina e-mail: firstname.lastname@example.org
3 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata, Buenos Aires, Argentina e-mail: email@example.com
Accepted: 14 March 2005
The effects of rapid rotation and bi-stability upon the density contrast between the equatorial and polar directions of a B[e] supergiant are re-investigated. Based on a new slow solution for different high rotational radiation-driven winds and the fact that bi-stability allows a change in the line-force parameters (α, k, and δ), the equatorial densities are about 102–104 times higher than the polar ones. These values are in qualitative agreement with the observations.
Key words: stars: early-type / stars: mass-loss / stars: rotation / stars: winds, outflows
© ESO, 2005
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