Rapidly rotating second-generation progenitors for the ‘blue hook’ stars of ω Centauri

Marco Tailo, Francesca D’Antona (), Enrico Vesperini, Marcella Di Criscienzo, Paolo Ventura, Antonino P. Milone, Andrea Bellini, Aaron Dotter, Thibaut Decressin, Annibale D’Ercole, Vittoria Caloi and Roberto Capuzzo-Dolcetta
Additional contact information
Marco Tailo: INAF-Osservatorio Astronomico di Roma
Francesca D’Antona: INAF-Osservatorio Astronomico di Roma
Enrico Vesperini: Indiana University
Marcella Di Criscienzo: INAF-Osservatorio Astronomico di Roma
Paolo Ventura: INAF-Osservatorio Astronomico di Roma
Antonino P. Milone: Research School of Astronomy and Astrophysics, Australian National University
Andrea Bellini: Space Telescope Science Institute
Aaron Dotter: Research School of Astronomy and Astrophysics, Australian National University
Thibaut Decressin: INAF-Osservatorio Astronomico di Roma
Annibale D’Ercole: INAF-Osservatorio Astronomico di Bologna
Vittoria Caloi: INAF, IAPS, Roma
Roberto Capuzzo-Dolcetta: Universitá degli Studi di Roma ‘La Sapienza’

Nature, 2015, vol. 523, issue 7560, 318-321

Abstract: The observed range of luminosities of the extremely hot ‘blue hook’ stars of the globular cluster ω Centauri is successfully explained by a model in which the progenitors of these stars are second-generation helium-rich stars characterized by a range of rotation rates arising during the cluster’s very early evolution.

Date: 2015
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DOI: 10.1038/nature14516

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