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dc.date.accessioned | 2020-04-21T18:16:19Z | |
dc.date.available | 2020-04-21T18:16:19Z | |
dc.date.issued | 2018-06 | |
dc.identifier.uri | http://sedici.unlp.edu.ar/handle/10915/93912 | |
dc.description.abstract | Most radiation-driven winds of massive stars can be modelled with m-CAK theory, resulting in the so-called fast solution. However, the most rapidly rotating stars among them, especially when the rotational speed is higher than ∼75 per cent of the critical rotational speed, can adopt a different solution, the so-called Ω-slow solution, characterized by a dense and slow wind. Here, we study the transition region of the solutions where the fast solution changes to the Ω-slow solution. Using both time-steady and time-dependent numerical codes, we study this transition region for various equatorial models of B-type stars. In all cases, in a certain range of rotational speeds we find a region where the fast and the Ω-slow solution can coexist. We find that the type of solution obtained in this co-existence region depends stongly on the initial conditions of our models. We also test the stability of the solutions within the co-existence region by performing base-density perturbations in the wind. We find that under certain conditions, the fast solution can switch to the Ω-slow solution, or vice versa. Such solution-switching may be a possible contributor of material injected into the circumstellar environment of Be stars, without requiring rotational speeds near critical values. | en |
dc.format.extent | 755-765 | es |
dc.language | en | es |
dc.subject | hydrodynamics | es |
dc.subject | stars: early-type | es |
dc.subject | stars: rotation | es |
dc.subject | stars: winds, outflows | es |
dc.title | Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars | en |
dc.type | Articulo | es |
sedici.identifier.uri | https://academic.oup.com/mnras/article/477/1/755/4975263 | es |
sedici.identifier.uri | https://ri.conicet.gov.ar/handle/11336/82696 | es |
sedici.identifier.other | http://dx.doi.org/10.1093/mnras/sty678 | es |
sedici.identifier.other | hdl:11336/82696 | es |
sedici.identifier.issn | 0035-8711 | es |
sedici.creator.person | Araya, I. | es |
sedici.creator.person | Curé, Michel | es |
sedici.creator.person | Doula, A. ud | es |
sedici.creator.person | Santillán, A. | es |
sedici.creator.person | Cidale, Lydia Sonia | es |
sedici.subject.materias | Astronomía | es |
sedici.description.fulltext | true | es |
mods.originInfo.place | Facultad de Ciencias Astronómicas y Geofísicas | es |
mods.originInfo.place | Instituto de Astrofísica de La Plata | es |
sedici.subtype | Articulo | es |
sedici.rights.license | Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) | |
sedici.rights.uri | http://creativecommons.org/licenses/by-nc-sa/4.0/ | |
sedici.description.peerReview | peer-review | es |
sedici.relation.journalTitle | Monthly Notices of the Royal Astronomical Society | es |
sedici.relation.journalVolumeAndIssue | vol. 477, no. 1 | es |