Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26..169c&link_type=abstract
XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S
Astronomy and Astrophysics
Astronomy
Scientific paper
The inclusion of rotation in the hydrodynamic equations of radiation driven winds in a rapidly rotating star yields to a new solution (Curé, M., 2004, ApJ, 614, 929). Combining this new solution (slow solution) and the standard solution (fast solution) to describe the wind structure of a rotating star, a hybrid wind model is obtained. The polar wind is described by the fast solution while the equatorial flow, by the slow solution. We compute simultaneously the line-force parameters and the density contrast between polar and equatorial regions. In the equatorial region close to the star ( < 2 R_*) we obtain density values 1000 times greater than the ones obtained in the polar region. In external regions the density contrast is around 10. We propose these solutions to explain the disk wind formation in B[e] stars. In the case of Be stars, the computed density contrast is between 10 and 30.
Cidale Lydia S.
Cure Michel
Rial Diego
Venero R.
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