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Mass loss implementation and temperature evolution of very massive stars

dc.contributorArmagh Observatory, and Planetarium, College Hill, Armagh BT61 9DG, N. Ireland, E-mail:
dc.contributorArmagh Observatory, and Planetarium, College Hill, Armagh BT61 9DG, N. Ireland, E-mail: ; Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
dc.contributor.authorSabhahit, Gautham N.
dc.contributor.authorVink, Jorick S.
dc.contributor.authorHiggins, Erin R.
dc.contributor.authorSander, Andreas A. C.
dc.date.accessioned2024-10-02T19:40:43Z
dc.date.available2024-10-02T19:40:43Z
dc.date.issued2023-01-01T00:00:00Z
dc.identifier.doi10.1017/S1743921322003623
dc.identifier.other2023IAUS..370..263S
dc.identifier.other10.1017/S1743921322003623
dc.identifier.other0000-0002-7442-1014
dc.identifier.other0000-0002-8445-4397
dc.identifier.other0000-0003-2284-4469
dc.identifier.other-
dc.identifier.urihttp://hdl.handle.net/20.500.14302/2104
dc.description.abstractVery massive stars (VMS) dominate the physics of young clusters due to their extreme stellar winds. The mass lost by these stars in their winds determine their evolution, chemical yields and their end fates. In this contribution we study the main-sequence evolution of VMS with a new mass-loss recipe that switches from optically-thin O star winds to optically-thick Wolf-Rayet type winds through the model independent transition mass loss.
dc.publisherWinds of Stars and Exoplanets
dc.titleMass loss implementation and temperature evolution of very massive stars
dc.typeinproceedings
dc.source.journalIAUS
dc.source.journalIAUS..370
dc.source.volume370
dc.identifier.bibcode2023IAUS..370..263S


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