The wind of rotating B supergiants - II. The δ-slow hydrodynamic regime

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dc.contributor.authorVenero, R. O. J.
dc.contributor.authorCure, M.
dc.contributor.authorPuls, J.
dc.contributor.authorCidale, L. S.
dc.contributor.authorHaucke, M.
dc.contributor.authorAraya, I.
dc.contributor.authorGormaz-Matamala, A.
dc.contributor.authorArcos, C.
dc.date.accessioned2025-01-20T16:12:28Z
dc.date.available2025-01-20T16:12:28Z
dc.date.issued2024
dc.description.abstractThe theory of line-driven winds can explain many observed spectral features in early-type stars, though our understanding the winds of B supergiants remains incomplete. The hydrodynamic equations for slowly rotating stellar winds predict two regimes based on the line-force parameter delta: the fast and the delta -slow solution. In this paper, we aim to explore the capability of the latter to explain the observed properties of B supergiant winds. We calculate H alpha line profiles, the most sensitive wind diagnostics in the optical, for both fast and delta -slow wind models. We fit them to observed data from a well-studied sample of B supergiants, by adapting the line-force parameters (k, alpha, and delta) of the hydrodynamic model. Unexpectedly, the observed H alpha spectra can be reproduced by both hydrodynamic wind regimes with similar precision. We argue that this similarity results from the similar shape of the normalized velocity law produced by both regimes in the lower, H alpha -forming wind region. Our findings raise a dichotomy, because mass-loss rates and terminal velocities (v(infinity)) for each solution are quite different. The delta -slow solution predicts maximum values for v(infinity) that are systematically lower than those measured in the ultraviolet, whereas the v(infinity) values of the fast solution are closer, and probably more appropriate. However, our results also indicate that the delta -slow solution might better describe the dense winds of B hypergiants. Multiwavelength analyses and a larger sample of stars are needed to reach a definitive conclusion.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stad3030
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stad3030
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/90335
dc.identifier.wosidWOS:001271977600001
dc.issue.numero1
dc.language.isoen
dc.pagina.final111
dc.pagina.inicio93
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjecthydrodynamics
dc.subjectstars: early-type
dc.subjectstars: mass-loss
dc.subjectstars: winds
dc.subjectoutflows
dc.titleThe wind of rotating B supergiants - II. The δ-slow hydrodynamic regime
dc.typeartículo
dc.volumen527
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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