Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-11-24T05:48:13.438Z Has data issue: false hasContentIssue false
  • English
  • Français

Calibration of the Pre-Main Sequence Binary System RS Cha: Impact of the Initial Chemical Mixture

Published online by Cambridge University Press:  09 August 2007

E. Alecian ,
Y. Lebreton ,
M.-J. Goupil ,
M.-A. Dupret  and
C. Catala
E. Alecian
Affiliation:
Observatoire de Paris, LESIA, CNRS UMR 8109 5 place Janssen, 92195 Meudon, France, email: [email protected]
Y. Lebreton
Affiliation:
Observatoire de Paris, GEPI, CNRS UMR 8111, 5 place Janssen, 92195 Meudon, France
M.-J. Goupil
Affiliation:
Observatoire de Paris, LESIA, CNRS UMR 8109 5 place Janssen, 92195 Meudon, France, email: [email protected]
M.-A. Dupret
Affiliation:
Observatoire de Paris, LESIA, CNRS UMR 8109 5 place Janssen, 92195 Meudon, France, email: [email protected]
C. Catala
Affiliation:
Observatoire de Paris, LESIA, CNRS UMR 8109 5 place Janssen, 92195 Meudon, France, 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.

Accurate observational data are available for the eclipsing double-lined spectroscopic binary system RS Cha, composed of two stars in the pre-main sequence stage of evolution: masses, radii, luminosities and effective temperatures of each component and metallicity of the system. This allows to build pre-main sequence stellar models representing the components of RS Cha and to constrain them in terms of physical ingredients, initial chemical composition and age.

We present stellar models we have calculated using the CESAM stellar evolution code for different sets of physical inputs (opacities, nuclear reaction rates, etc.) and different initial parameters (global metallicity, helium abundance, individual abundances of heavy elements). We discuss their ability to reproduce the observational constraints simultaneously for the two components. We focus on the impact on the models of the chemical mixture adopted and we propose a calibration for the RS Cha system providing an estimate of its age and initial helium abundance.

Keywords

stars: pre–main-sequencestars: interiorsbinaries: generalSun: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S240: Binary Stars as Critical Tools & Tests in Contemporary Astrophysics , August 2006 , pp. 652 - 657
Copyright
Copyright © International Astronomical Union 2007

References

Alecian, E., Catala, C., van't Veer-Menneret, C., Goupil, M.-J., & Balona, L. 2005, A&A, 442, 993 (paper I)Google Scholar
Alecian, E., Goupil, M.-J., Lebreton, Y., Dupret, M.-A., & Catala, C. 2006, A&A, acceptedGoogle Scholar
Alexander, D.R. & Ferguson, J.W. 1994, ApJ, 437, 879 CrossRefGoogle Scholar
Angulo, C., Arnould, M., Rayet, M., et al. 1999, Nuclear Physics A, 656, 3 CrossRefGoogle Scholar
Asplund, M., Grevesse, N., & Sauval, A.J. 2005b, in ASP Conf. Ser. 336: Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis, ed. T.G. Barnes, III & F.N. Bash, 25Google Scholar
Asplund, M., Grevesse, N., Sauval, A.J., Allende Prieto, C., & Blomme, R. 2005a, A&A, 431, 693 Google Scholar
Asplund, M., Grevesse, N., Sauval, A.J., Allende Prieto, C., & Kiselman, D. 2004, A&A, 417, 751 Google Scholar
Böhm-Vitense, E. 1958, Zeitschrift Astrophysics, 46, 108 Google Scholar
Clausen, J.V. & Nordstrom, B. 1980, A&A, 83, 339 Google Scholar
Grevesse, N. & Noels, A. 1993, Origin and Evolution of the Elements, ed. Prantzos, N., Langioni-flam, E., & Classe, M. (Cambridge Univ. Press), p. 14 Google Scholar
Mamajek, E.E., Lawson, W.A., & Feigelson, E.D. 2000, ApJ, 544, 356 CrossRefGoogle Scholar
Morel, P. 1997, A&AS, 124, 597 Google Scholar
Ribas, I., Jordi, C., Torra, J., & Giménez, Á. 2000, MNRAS, 313, 99 CrossRefGoogle Scholar