Hostname: page-component-586b7cd67f-dsjbd Total loading time: 0 Render date: 2024-11-30T20:33:17.570Z Has data issue: false hasContentIssue false
  • English
  • Français

Mass loss of different stellar populations in globular clusters

Published online by Cambridge University Press:  11 March 2020

Marco Tailo Open the ORCID record for Marco Tailo [Opens in a new window]
Marco Tailo*
Affiliation:
Dipartimento di Fisica e Astronomia “Galileo Galilei”, Univ. di Padova,Vicolo dell’Osservatorio 3, Padova, IT-35122 emails: [email protected], [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Once the age and metallicity are fixed, the colour distribution of horizontal branch stars in a globular cluster depends on few parameters: the helium abundance of the population and the mass lost during the pre-HB stages. These parameters are usually derived from the HB itself, hence they are degenerate. Breaking this degeneracy and understanding their role is a tricky and challenging problem that no study has solved yet. Combining the information obtained from the chromosome maps and the analysis of multi-band photometry with state of the art stellar evolution models, we can obtain a solid estimate of Y for the various stellar populations in a GC. We will then have, for the first time, the possibility to break the parameters’ degeneracy on the HB, understand the role of the mass loss, and lay the foundation to build another piece of the multiple populations mosaic.

Keywords

stars: Hertzsprung-Russell diagramstars: horizontal-branchstars: mass lossglobular clusters: individual (NGC5272, NGC6121)stars: fundamental parameters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 341 - 345
Copyright
© International Astronomical Union 2020

References

Benkö, J. M., Bakos, G. Á., & Nuspl, J., 2006, MNRAS, 372, 1657CrossRefGoogle Scholar
D’Antona, F., Caloi, V. R.et al. 2002, A&A, 395, 69Google Scholar
Iben, I. & Renzini, A. 1984, PhR, 105, 329Google Scholar
Marino, A. F., Villanova, S., Piotto, G., et al. 2008, A&A, 490, 625Google Scholar
Marino, A. F., Villanova, S., Milone, A. P., et al. 2011, ApJl, 730, L16CrossRefGoogle Scholar
Milone, A. P., Piotto, G., Bedin, L. R., et al. 2012, ApJ, 744, 58CrossRefGoogle Scholar
Milone, A. P., Marino, A. F., Bedin, L. R., et al. 2014, MNRAS, 439, 1588CrossRefGoogle Scholar
Milone, A. P., Piotto, G., Renzini, A., et al. 2017, MNRAS, 464, 3636CrossRefGoogle Scholar
Milone, A. P.et al. 2018, MNRAS, 481, 5098CrossRefGoogle Scholar
Tailo, M., Milone, A. P., Marino, A. F.et al. 2019a, ApJ, 873, 123CrossRefGoogle Scholar
Tailo, M., D’Antona, F., Caloi, V.et al. 2019b, MNRAS, 486, 5895CrossRefGoogle Scholar