Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
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-...
| Autores: | ; ; |
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| Tipo de documento: | Artículo |
| Estado: | Published version |
| Fecha de publicación: | 2005 |
| País: | Argentina |
| Institución: | Consejo Nacional de Investigaciones Científicas y Técnicas |
| Repositorio: | CONICET Digital (CONICET) |
| Lenguaje: | Inglés |
| OAI Identifier: | oai:ri.conicet.gov.ar:11336/38103 |
| Acceso en línea: | http://hdl.handle.net/11336/38103 |
| Nivel de acceso: | Acceso abierto |
| Palabra clave: | Early type stars Mass loss Rotation of stars Star winds Outflows https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| Sumario: | 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 10^2-104 times higher than the polar ones. These values are in qualitative agreement with the observations. |
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