Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-22T18:02:42.138Z Has data issue: false hasContentIssue false
  • English
  • Français

The Chemical Evolution of Omega Centauri

Published online by Cambridge University Press:  01 December 2006

Donatella Romano
Donatella Romano*
Affiliation:
INAF–Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127, Bologna, Italy email: [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.

The globular cluster ω Cen is an outstanding object in terms of both its chemical and kinematic properties. Its large mass, spread in element abundances, chemical and kinematical segregations, as well as its peculiar orbit, all suggest that it is the surviving remnant of a larger system. In this contribution we deal with the chemical evolution of ω Cen in the framework of a model where it is the remnant of a dwarf spheroidal galaxy evolved in isolation and then swallowed and partially disrupted by the Milky Way. Both infall of primordial matter and metal-enriched gas outflows are necessary in order to reproduce the observed stellar metallicity distribution function, age-metallicity relation and several abundance ratios. Yet, as long as an ordinary stellar initial mass function and standard stellar yields are adopted, we fail by far to get the enormous helium enhancement required to explain the double main sequence of ω Cen.

Keywords

Galaxies: dwarfgalaxies: evolutionglobular cluster: individual (ω Centauri)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 258 - 259
Copyright
Copyright © International Astronomical Union 2007

References

Hilker, M., Kayser, A., Richtler, T., & Willemsen, P. 2004, A&A 422, L9Google Scholar
Ikuta, C. & Arimoto, N. 2000, A&A 358, 535Google Scholar
Norris, J. E. 2004, ApJ 612, L25CrossRefGoogle Scholar
Piotto, G. et al. , 2005, ApJ 621, 777Google Scholar
Romano, D., Matteucci, F., Tosi, M., Pancino, E., Bellazzini, M., Ferraro, F.R., Limongi, M., & Sollima, A. 2007, MNRAS in press (astro-ph/0701162)Google Scholar
Salpeter, E. E. 1955, ApJ 121, 161CrossRefGoogle Scholar
Sollima, A., Ferraro, F. R., Pancino, E., & Bellazzini, M. 2005, MNRAS 357, 265CrossRefGoogle Scholar
Sollima, A., Borissova, J., Catelan, M., Smith, H. A., Minniti, D., Cacciari, C., & Ferraro, F. R. 2006, ApJ 640, L43CrossRefGoogle Scholar
Stanford, L. M., DaCosta, G. S. Costa, G. S., Norris, J. E., & Cannon, R. D. 2006, ApJ 647, 1075CrossRefGoogle Scholar