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Simulation of a Hydrodynamic Stellar Wind from a Rapidly Rotating Star

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dc.contributor.authorBogovalov, S. V.
dc.contributor.authorRomanikhin, S. M.
dc.contributor.authorTronin, I. V.
dc.contributor.authorБоговалов, Сергей Владимирович
dc.contributor.authorТронин, Иван Владимирович
dc.date.accessioned2024-11-20T11:17:53Z
dc.date.available2024-11-20T11:17:53Z
dc.date.issued2019
dc.description.abstract© 2019, Pleiades Publishing, Inc. The mechanism for the formation of disk-like flows from rapidly rotating Be stars is not yet clear. An axisymmetric hydrodynamic stellar wind flow from a rapidly rotating star has been simulated numerically as a step in solving this problem. The change in the shape of the star as it rotates and the turbulence excited in the stellar wind at Reynolds numbers ∼10 9 −10 13 are taken into account. Calculations show the formation of a disk-like flow from the stellar surface at the equator, which expands into the polar regions due to a pressure gradient on scales of the order of the stellar radius. A poloidal velocity vortex is formed at high latitudes. No turbulence is excited near the equator within the simplest standard models and, therefore, no quasi-Keplerian disk-like flow emerges in the equatorial plane. A dependence of the total mass flux on the stellar rotation rate at various surface temperatures has been obtained.
dc.format.extentС. 81-91
dc.identifier.citationBogovalov, S. V. Simulation of a Hydrodynamic Stellar Wind from a Rapidly Rotating Star / Bogovalov, S.V., Romanikhin, S.M., Tronin, I.V. // Astronomy Letters. - 2019. - 45. - № 2. - P. 81-91. - 10.1134/S1063773719020026
dc.identifier.doi10.1134/S1063773719020026
dc.identifier.urihttps://www.doi.org/10.1134/S1063773719020026
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dc.identifier.urihttp://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcAuth=Alerting&SrcApp=Alerting&DestApp=WOS_CPL&DestLinkType=FullRecord&UT=WOS:000466737800004
dc.identifier.urihttps://openrepository.mephi.ru/handle/123456789/16939
dc.relation.ispartofAstronomy Letters
dc.titleSimulation of a Hydrodynamic Stellar Wind from a Rapidly Rotating Star
dc.typeArticle
dspace.entity.typePublication
oaire.citation.issue2
oaire.citation.volume45
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