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Very Massive Stars: Near and Far

Published online by Cambridge University Press:  29 August 2024

Sébastien Martinet Open the ORCID record for Sébastien Martinet [Opens in a new window] ,
Georges Meynet ,
Sylvia Ekström ,
Cyril Georgy ,
Lionel Haemmerlé ,
Devesh Nandal Open the ORCID record for Devesh Nandal [Opens in a new window]  and
Raphael Hirschi
Sébastien Martinet*
Affiliation:
Geneva Observatory, University of Geneva, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
Georges Meynet
Affiliation:
Geneva Observatory, University of Geneva, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
Sylvia Ekström
Affiliation:
Geneva Observatory, University of Geneva, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
Cyril Georgy
Affiliation:
Geneva Observatory, University of Geneva, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
Lionel Haemmerlé
Affiliation:
Geneva Observatory, University of Geneva, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
Devesh Nandal
Affiliation:
Geneva Observatory, University of Geneva, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
Raphael Hirschi
Affiliation:
Astrophysics Group, Keele University, Keele, Staffordshire, ST5 5BG, UK Institute for Physics and Mathematics of the Universe (WPI), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa 277-8583, Japan
*
email: sebastien.martinet@unige.ch
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Abstract

In addition to being spectacular objects, very massive stars (VMS) are suspected to have a tremendous impact on their environment and on the whole cosmic evolution. The nucleosynthesis both during their advanced stages and their final explosion likely contribute greatly to the overall enrichment of the Universe. Their resulting Supernovae are candidates for the most superluminous events and their extreme conditions lead also to very important radiative and mechanical feedback effects, from local to cosmic scale. With the recent implementation of a new equation of state in the GENEC stellar evolution code, appropriate for describing the conditions in the central regions of very massive stars in the advanced phases, we present new results on VMS evolution from Population III to solar metallicity. We explore their evolution and final fate as potential (P)PISNe across the cosmic time. We compare our results to recent spectroscopic observations of VMS in the Large Magellanic Cloud (LMC). We also underline the important radiative feedback of Population III VMS during the reionization epoch and the chemical contribution of these stars at high metallicity, especially for short-lived radionuclei.

Keywords

stars: evolutionstars: supernovaestars: fundamental parameters
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 369 - 375
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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