Hostname: page-component-7c8c6479df-xxrs7 Total loading time: 0 Render date: 2024-03-29T09:54:20.444Z Has data issue: false hasContentIssue false

Radiation driven winds with rotation: the oblate finite disc correction factor

Published online by Cambridge University Press:  12 July 2011

Ignacio Araya
Affiliation:
Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile
Michel Curé
Affiliation:
Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile
Anahí Granada
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina
Lydia S. Cidale
Affiliation:
Instituto de Astrofísica La Plata, CCT La Plata-CONICET-UNLP, Argentina
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have incorporated the oblate distortion of the shape of the star due to the stellar rotation, which modifies the finite disk correction factor (fD) in the m-CAK hydrodynamical model. We implement a simplified version for the fD allowing us to solve numerically the non–linear m-CAK momentum equation. We solve this model for a classical Be star in the polar and equatorial directions. The star's oblateness modifies the polar wind, which is now much faster than the spherical one, mainly because the wind receives radiation from a larger (than the spherical) stellar surface. In the equatorial direction we obtain slow solutions, which are even slower and denser than the spherical ones. For the case when the stellar rotational velocity is about the critical velocity, the most remarkable result of our calculations is that the density contrast between the equatorial density and the polar one, is about 100. This result could explain a long-standing problem on Be stars.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Curé, M. 2004, ApJ, 614, 929Google Scholar
Lamers, H. J. G. L. M. & Waters, L. B. F. M. 1987, A&A, 182, 80Google Scholar
Pelupessy, I., Lamers, H. J. G. L. M., & Vink, J. S. 2000, A&A, 359, 695Google Scholar
Slettebak, A., Kuzma, T. J. & Collins, G. W. II 1980, ApJ, 242, 171CrossRefGoogle Scholar
Townsend, R. H. D., Owocki, S. P., & Howarth, I. D. 2004, MNRAS, 350, 189CrossRefGoogle Scholar