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Chemical abundances of fast-rotating OB stars

  • Constantin Cazorla (a1), Thierry Morel (a1), Yaël Nazé (a1) and Gregor Rauw (a1)

Abstract

Fast rotation in massive stars is predicted to induce mixing in their interior, but a population of fast-rotating stars with normal nitrogen abundances at their surface has recently been revealed (Hunter et al.2009; Brott et al.2011, but see Maeder et al.2014). However, as the binary fraction of these stars is unknown, no definitive statements about the ability of single-star evolutionary models including rotation to reproduce these observations can be made. Our work combines for the first time a detailed surface abundance analysis with a radial-velocity monitoring for a sample of bright, fast-rotating Galactic OB stars to put strong constraints on stellar evolutionary and interior models.

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References

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Brott, I., Evans, C. J., Hunter, I., et al. 2011, A&A 530, A116
Georgy, C., Ekström, S., Granada, A., et al. 2013, A&A 553, A24
Hunter, I., Brott, I., Langer, N., et al. 2009, A&A 496, 841
Maeder, A., Przybilla, N., Nieva, M.-F., et al. 2014, A&A 565, A39
Rauw, G., Morel, T., & Palate, M. 2012, A&A 546, A77
Ritchie, B. W., Stroud, V. E., Evans, C. J., et al. 2012, A&A 537, A29
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