The first stellar generation in globular clusters may have contained
low-metallicity massive stars. We modelled the evolution of such stars
with masses 100-600 Msun and found that they evolve into cool
supergiants. These supergiants are particular because they spend not
only their helium-burning phase, but even the last 15% of their
core-hydrogen-burning phase on the supergiant branch. Their wind
therefore contains hot-hydrogen-burning products. Due to the presence
of hot massive TWUIN stars in the cluster at the same time, the winds
can be trapped in photoionization-confined shells. We simulate the
shell formation and show that gravitational instabilities lead to star
formation. We propose a scenario in which these shells form the second
generation low-mass stars in globular clusters with anomalous surface
abundances.
Related publication:
http://adsabs.harvard.edu/abs/2017arXiv171104007S
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