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Massive Oe/Be stars at low metallicity: candidate progenitors of long GRBs?

Martayan, Christophe ; Baade, Dietrich ; Zorec, Juan ; Frémat, Yves ; Fabregat, Juan ; Ekström, Sylvia

In: Proceedings of the International Astronomical Union, 2010, vol. 6, no. S272, p. 300-301

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    Titel
    • Massive Oe/Be stars at low metallicity: candidate progenitors of long GRBs?
    Autor
    • Martayan, Christophe. ESO, Chile
    • Baade, Dietrich. ESO, Germany
    • Zorec, Juan. Instritut d'Astrophysique de Paris, France
    • Frémat, Yves. Royal Observatory of Belgium, Brussels, Belgium
    • Fabregat, Juan. Valencia University, Spain
    • Ekström, Sylvia. Geneva Observatory, Switzerland
    Dokumententyp
    • Postprint
    Sprache
    • Englisch
    Veröffentlicht in
    • Proceedings of the International Astronomical Union, 2010, vol. 6, no. S272, p. 300-301. Cambridge University Press
    Andere elektronische Ausgabe
    OAI-PMH-ID
    • oai:doc.rero.ch:295908
    Summary
    At low metallicity B-type stars rotate faster than at higher metallicity, typically in the SMC. As a consequence, a larger number of fast rotators is expected in the SMC than in the Galaxy, in particular more Be/Oe stars. With the ESO-WFI in its slitless mode, we examined the SMC open clusters and found an occurence of Be stars 3 to 5 times larger than in the Galaxy. The evolution of the angular rotational velocity seems to be the main key on the understanding of the specific behaviour and stellar evolution of such stars at different metallicities. With the results of this WFI study and using observational clues on the SMC WR stars and massive stars, as well as the theoretical indications of long gamma-ray burst progenitors, we identify the low metallicity massive Be and Oe stars as potential LGRB progenitors. Therefore the expected rates and numbers of LGRB are calculated and compared to the observed ones, leading to a good probability that low metallicity Be/Oe stars are actually LGRB progenitors