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Unraveling massive star and binary physics in the nearby low-Z galaxy SMC as a proxy for high-redshift galaxies

Published online by Cambridge University Press:  29 August 2024

Daniel Pauli Open the ORCID record for Daniel Pauli [Opens in a new window]
Daniel Pauli*
Affiliation:
Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, 14476 Potsdam, Germany
*
email: dpauli@astro.physik.uni-potsdam.de
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Abstract

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Low metallicity (Z) massive stars are among the main feedback agents in the early Universe and in present-day blue dwarf galaxies. The nearby star-forming SMC galaxy offers conditions which resemble those at redshift z∼2 i.e. where modern galaxies formed and star formation peaked. Here we present the recent results about the nature of the eclipsing O-type binary in the SMC, AzV 476, to gain insights on the properties of massive stars and binaries at earlier cosmic epochs. We find that the primary has surprisingly low mass while being much brighter and hotter than the secondary. To place the measured stellar properties in the evolutionary context we modeled the system and confirm that AzV 476 is a post-interaction binary with the primary already being core helium (He) burning, while still having a hydrogen-rich (H-rich) envelope. These results constrain massive binary evolutionary scenarios and guide the searches of stripped stars in low-Z environments.

Keywords

binaries: closebinaries: eclipsingbinaries: spectroscopicstars: early-typestars: fundamental parametersstars: individual: AzV 476Magellanic Clouds
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 116 - 118
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Klencki, J., Istrate, A. G., Nelemans, G., & Pols, O. 2021, arXiv, 2111.10271Google Scholar
Pauli, D., and Oskinova, L. M., Hamann, W.-R., Ramachandran, V., Todt, H., Sander, A. A. C., Shenar, T., Rickard, M., Maz Apellániz, J. & Prinja, R. 2022, A&A, A9, 659Google Scholar
Ramachandran, V., Hamann, W.-R., Oskinova, L. M., Gallagher, J. S., Hainich, R., Shenar, T., Sander, A. A. C., Todt, H. & Fulmer, L. 2019, A&A, A104, 625 Google Scholar
Weidner, C. & Vink, J. S. 2010, A&A, A98, 524 Google Scholar