Astron. Astrophys. 343, 261-265 (1999)

Metal abundances of A-type stars in galactic clusters ^*

III. Persei: new results

A. Hui-Bon-Hoa

Laboratoire d'Astrophysique Extragalactique et de Cosmologie, CNRS-(URA 173), Observatoire de Paris, Université Paris 7, DAEC, Observatoire de Meudon, F-92195 Meudon Cedex, France

Received 21 August 1998 / Accepted 17 November 1998

Abstract

We complete our study (Hui-Bon-Hoa et al. 1997) of the abundances of Mg, Ca, Sc, Cr, Fe, and Ni in  Per cluster stars using new spectra of two stars of the previous sample and also adding two more objects. The new spectra of BD  and HD 21527 show that the former has an almost solar composition whereas the latter is an Am star with the iron peak elements being all enhanced and Ca marginally underabundant. As for the additional stars of this study, HD 19954 has a pattern very close to solar, and HD 20135 is an SB2 system where both components seem to be Am stars: Ca and Sc are strongly deficient; Cr and Ni are overabundant in one component. A more thorough study is needed for confirmation.

Key words: stars: abundances stars: chemically peculiar Galaxy: open clusters and associations: individual:

* Based on observations collected at the Observatoire de Haute-Provence (France)

Send offprint requests to: A. Hui-Bon-Hoa

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Contents

• 1. Introduction
• 2. Observations and reductions
  • 2.1. The sample
  • 2.2. Data collection and reduction
• 3. Analysis
  • 3.1. Effective temperature and surface gravity
  • 3.2. Abundance determinations
• 4. Results
• 5. Discussion
• Acknowledgements
• References

© European Southern Observatory (ESO) 1999

Online publication: March 1, 1999
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