Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-19T10:09:21.094Z Has data issue: false hasContentIssue false
  • English
  • Français

Abundances of A/F and Am/Fm stars in open clusters as constraints to self-consistent models including transport processes

Published online by Cambridge University Press:  02 March 2005

Richard Monier  and
Olivier Richard
Richard Monier
Affiliation:
GRAAL, Universite Montpellier II, Place E. Bataillon, 34095 Montpellier, France email: [email protected], [email protected]
Olivier Richard
Affiliation:
GRAAL, Universite Montpellier II, Place E. Bataillon, 34095 Montpellier, France email: [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.

We describe the current status of a programme we started a few years ago to observe a large number of A/F and Am/Fm stars in open clusters of various ages. Spectra were obtained with the AURELIE and ELODIE spectrographs at a resolving power of about 40000 and $S/N$ ratios from 100 up to 500. Abundances of 11 chemical elements have been derived by using Takeda's (1995) procedure. A short review on previous abundance determinations of A and F dwarfs in open clusters and a progress report on the current status of this project are presented. New abundance determinations for 24 A and F dwarfs in the Coma Berenices cluster are presented. These abundance determinations serve to set constraints to self-consistent evolutionary models of A and F stars including transport processes.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Diffusionstars: abundancesstars: chemically peculiaropen clusters and associations: individual: (Coma Ber)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 209 - 214
Copyright
© 2004 International Astronomical Union