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Mass loss implementation and temperature evolution of very massive stars

Published online by Cambridge University Press:  16 August 2023

Gautham N. Sabhahit Open the ORCID record for Gautham N. Sabhahit [Opens in a new window] ,
Jorick S. Vink Open the ORCID record for Jorick S. Vink [Opens in a new window] ,
Erin R. Higgins Open the ORCID record for Erin R. Higgins [Opens in a new window]  and
Andreas A.C. Sander
Gautham N. Sabhahit
Affiliation:
Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, N. Ireland, E-mail: [email protected]
Jorick S. Vink
Affiliation:
Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, N. Ireland, E-mail: [email protected]
Erin R. Higgins
Affiliation:
Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, N. Ireland, E-mail: [email protected]
Andreas A.C. Sander
Affiliation:
Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, N. Ireland, E-mail: [email protected] Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
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Abstract

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Very 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.

Keywords

stars: mass lossstars: windsoutflowsstars: evolution
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S370: Winds of Stars and Exoplanets , August 2021 , pp. 263 - 268
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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