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Testing how massive stars evolve, lose mass, and collapse at low metal content

Published online by Cambridge University Press:  30 December 2019

Eliceth Y. Rojas Montes  and
Jorick Vink
Eliceth Y. Rojas Montes
Affiliation:
School of Mathematics and Physics, Queen’s University Belfast, Belfast, BT7 1NN, Northern Ireland email: eliceth.rojasmontes@armagh.ac.uk Armagh Observatory and Planetarium, Armagh, BT61 9DG, Northern Ireland email: jorick.vink@armagh.ac.uk
Jorick Vink
Affiliation:
Armagh Observatory and Planetarium, Armagh, BT61 9DG, Northern Ireland email: jorick.vink@armagh.ac.uk
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Abstract

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In order to test massive star evolution above 25 M⊙, we perform spectral analysis on a sample of massive stars in the Small Magellanic Cloud that includes both O stars as well as more evolved Wolf-Rayet stars. We present a grid of non-LTE stellar atmospheres that has been calculated using the cmfgen code, in order to have a systematic and homogeneous approach. We obtain stellar and wind parameters for O stars, spectral types ranging from O2 to O6, and the complete sample of known Wolf-Rayet stars. We discuss the evolutionary status of both the O and WR stars and the links between them, as well as the most likely evolutionary path towards black hole formation in a low metallicity environment, including testing theoretical predictions for mass-loss rates at low metallicities.

Keywords

stars: early-typestars:Wolf-RayetSmall Magellanic Cloudstars: fundamental parameters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 98 - 101
Copyright
© International Astronomical Union 2019 

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