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Core-hydrogen-burning RSGs in the early globular clusters

Published online by Cambridge University Press:  27 October 2016

Dorottya Szécsi
Affiliation:
Argelander-Institut für Astronomie, Auf dem Hügel 71, Bonn-53121, Germany email: [email protected], [email protected]
Jonathan Mackey
Affiliation:
I. Physikalisches Institut, Universität zu Köln, Zülpicher Straße 77, 50937 Köln, Germany email: [email protected]
Norbert Langer
Affiliation:
Argelander-Institut für Astronomie, Auf dem Hügel 71, Bonn-53121, Germany email: [email protected], [email protected]
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Abstract

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The first stellar generation in galactic globular clusters contained massive low-metallicity stars (Charbonnel et al. 2014). We modelled the evolution of this massive stellar population and found that such stars with masses 100-600 M evolve into cool RSGs (Szécsi et al. 2015). These RSGs spend not only the core-He-burning phase but even the last few 105 years of the core-H-burning phase on the SG branch. Due to the presence of hot massive stars in the cluster at the same time, we show that the RSG wind is trapped into photoionization confined shells (Mackey et al. 2014). We simulated the shell formation around such RSGs and find them to become gravitationally unstable (Szécsi et al. 2016). We propose a scenario in which these shells are responsible for the formation of the second generation low-mass stars in globular clusters with anomalous surface abundances.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2016 

References

Charbonnel, C., Chantereau, W., Krause, M., Primas, F., & Wang, Y. 2014, A&A, 569, L6 Google Scholar
Mackey, J., Mohamed, S., Gvaramadze, V. V. et al. 2014, Nature, 512, 282 Google Scholar
Szécsi, D., Langer, N., Yoon, S.-C. et al. 2015, A&A, 581, A15 Google Scholar
Szécsi, D., Mackey, J., & Langer, N. 2016, in preparation Google Scholar