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Winds from fast rotating stars

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dc.contributor.authorBogovalov, S. V.
dc.contributor.authorPetrov, M. A.
dc.contributor.authorTimofeev, V. A.
dc.contributor.authorБоговалов, Сергей Владимирович
dc.contributor.authorПетров, Максим Александрович
dc.date.accessioned2024-11-29T16:44:05Z
dc.date.available2024-11-29T16:44:05Z
dc.date.issued2021
dc.description.abstractNumerical modelling of an isothermal wind from a fast rotating star is performed. Excitation of hydrodynamical turbulence and deviation of the shape of the stellar surface from a sphere are taken into account. Rotation and turbulence result in a dramatic increase of the mass flow rate from the star in comparison with a non-rotating one. The outflow occurs predominantly from a region on the stellar surface located at the equator. This flow expands rapidly due to thermal pressure. However, a disc-like flow at the equator is formed. The flow is more complicated near the pole. At large distances from the star a radially expanding wind is formed while close to the star some fraction of the outflow from the equatorial region falls down on to the stellar surface, producing a huge vortex. The dependence of the mass loss rate on the parameters of the star is presented.
dc.format.extentС. 2409-2418
dc.identifier.citationBogovalov, S. V. Winds from fast rotating stars / Bogovalov, SV, Petrov, MA, Timofeev, VA // Monthly Notices of the Royal Astronomical Society. - 2021. - 502. - № 2. - P. 2409-2418. - 10.1093/mnras/stab036
dc.identifier.doi10.1093/mnras/stab036
dc.identifier.urihttps://www.doi.org/10.1093/mnras/stab036
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dc.identifier.urihttps://openrepository.mephi.ru/handle/123456789/24247
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleWinds from fast rotating stars
dc.typeArticle
dspace.entity.typePublication
oaire.citation.issue2
oaire.citation.volume502
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