Radiative driven MHD wind solutions for Wolf-Rayet stars
A solution for the Wolf-Rayet stars wind is obtained by solving the MHD equations combined with the radiative driven winds formalism. In this model we combine radiation pressure, collimated magnetic fields and centrifugal forces. Non- isotropic mass density distribution is introduced through an exte...
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| Autores principales: | , |
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| Formato: | Articulo Comunicacion |
| Lenguaje: | Español |
| Publicado: |
1994
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/154928 |
| Aporte de: |
| Sumario: | A solution for the Wolf-Rayet stars wind is obtained by solving the MHD equations combined with the radiative driven winds formalism. In this model we combine radiation pressure, collimated magnetic fields and centrifugal forces. Non- isotropic mass density distribution is introduced through an external mass asymmetry parameter. This formalism can be applied not only to Wolf-Rayet stars but also to early B stars and naturally includes late B stars for which radiation pressure in not dominant. We discuss the different assumptions needed to solve the dynamical equations. The terminal velocity dependence of the wind on the magnetic field strength, mass density anisotropy and rotation is discussed. |
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