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Modeling of the wind/disk outflow from be stars

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dc.contributor.authorBogovalov, S.
dc.contributor.authorPetrov, M.
dc.contributor.authorБоговалов, Сергей Владимирович
dc.contributor.authorПетров, Максим Александрович
dc.date.accessioned2024-11-29T21:18:37Z
dc.date.available2024-11-29T21:18:37Z
dc.date.issued2021
dc.description.abstract© 2021 by the authors. Licensee MDPI, Basel, Switzerland.The objective of this work is to reproduce the formation of the fast polar wind and viscous disk outflow from Be stars in a unified physical picture. Numerical modeling of the plasma outflow from fast rotating stars was performed taking into account the acceleration of the plasma due to scattering of the radiation of the star in lines of plasma ions and excitation of the hydrodynamic turbulence in the outflow. The fast polar wind naturally arises in this picture with an expected flow rate. For the first time, it is shown that a disk-like outflow with a relatively high level of turbulence is formed at the equator of fast rotating stars emitting radiation-driven wind. However, the level of turbulent viscosity is well below the level necessary for the formation of a Keplerian disk.
dc.identifier.citationBogovalov, S. Modeling of the wind/disk outflow from be stars / Bogovalov, S., Petrov, M. // Universe. - 2021. - 7. - № 10. - 10.3390/universe7100353
dc.identifier.doi10.3390/universe7100353
dc.identifier.urihttps://www.doi.org/10.3390/universe7100353
dc.identifier.urihttps://www.scopus.com/record/display.uri?eid=2-s2.0-85116690269&origin=resultslist
dc.identifier.urihttp://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcAuth=Alerting&SrcApp=Alerting&DestApp=WOS_CPL&DestLinkType=FullRecord&UT=WOS:000726384400001
dc.identifier.urihttps://openrepository.mephi.ru/handle/123456789/24789
dc.relation.ispartofUniverse
dc.titleModeling of the wind/disk outflow from be stars
dc.typeArticle
dspace.entity.typePublication
oaire.citation.issue10
oaire.citation.volume7
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