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Issue A&A
Volume 437, Number 3, July III 2005
Page(s) 929 - 933
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20052686



A&A 437, 929-933 (2005)
DOI: 10.1051/0004-6361:20052686

Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds

M. Curé1, D. F. Rial2 and L. Cidale3

1  Departamento de Física y Meteorología, Facultad de Ciencias, Universidad de Valparaíso, Valparaíso, Chile
    e-mail: michel.cure@uv.cl
2  Departamento de Matemáticas, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina
    e-mail: drial@dm.uba.ar
3  Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata, Buenos Aires, Argentina
    e-mail: lydia@fcaglp.unlp.edu.ar

(Received 11 November 2004 / Accepted 14 March 2005)

Abstract
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 ($\alpha$, k, and $\delta$), 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

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© ESO 2005


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