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

dc.creatorCure, M.
dc.creatorRial, D.
dc.creatorCidale, Lydia Sonia
dc.date.accessioned2018-03-07T13:19:55Z
dc.date.accessioned2018-11-06T14:29:47Z
dc.date.available2018-03-07T13:19:55Z
dc.date.available2018-11-06T14:29:47Z
dc.date.created2018-03-07T13:19:55Z
dc.date.issued2005-07
dc.identifierCure, M.; Rial, D.; Cidale, Lydia Sonia; Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds; EDP Sciences; Astronomy and Astrophysics; 437; 3; 7-2005; 929-933
dc.identifier0004-6361
dc.identifierhttp://hdl.handle.net/11336/38103
dc.identifierCONICET Digital
dc.identifierCONICET
dc.identifier.urihttp://repositorioslatinoamericanos.uchile.cl/handle/2250/1887056
dc.description.abstractThe 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.
dc.languageeng
dc.publisherEDP Sciences
dc.relationinfo:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361:20052686
dc.relationinfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2005A%26A...437..929C
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.rightsinfo:eu-repo/semantics/openAccess
dc.subjectEarly type stars
dc.subjectMass loss
dc.subjectRotation of stars
dc.subjectStar winds
dc.subjectOutflows
dc.titleOutflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds
dc.typeArtículos de revistas
dc.typeArtículos de revistas
dc.typeArtículos de revistas


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