Hostname: page-component-84b7d79bbc-rnpqb Total loading time: 0 Render date: 2024-08-01T15:22:42.287Z Has data issue: false hasContentIssue false
  • English
  • Français

Carbon Depletion in Case B Mass Transfer Algol-Type Binaries

Published online by Cambridge University Press:  07 August 2017

Tae S. Yoon  and
Kent Honeycutt
Tae S. Yoon
Affiliation:
Kyungpook National University Dept. of Astronomy and Meteorology Taegu 702-701 KOREA (South)
Kent Honeycutt
Affiliation:
Indiana University Astronomy Department Bloomington, IN 47405 U.S.A.

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 surface carbon abundances of Algol secondaries are known to be low compared to field stars of similar type. The C and N anomalies of these G and K subgiants are undoubtedly due to the exposure of CN cycle processed material as mass transfer removes the outer layers of the star. Therefore the carbon abundance is a promising tool for helping fix the evolutionary state of Algols, particularly the amount of mass which has been lost from the secondary. We report here the carbon abundance of 12 Algol secondaries as deduced from the g-band in spectra obtained during photometric totality. We compare the abundances to those from models of single stars of appropriate age and mass. The values of log ∊(C) for this sample fall 0.25–0.75 dex below field G and K giants, and 1.25–1.75 dex above “stripped” single star models. This larger sample supports the conclusions of Parthasarthy et al. regarding mixing and mass loss, which they deduced from a smaller sample of carbon abundances.

Type
Oral and Contributed Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 355 - 358
Copyright
Copyright © Kluwer 1992 

References

Balachandran, S., Lambert, D.L., Tomkin, J. and Parthasarathy, M. 1986, M.N.R.A.S. 219, 479.Google Scholar
Brancewicz, H.K., and Dworak, T.Z. 1980, Acta Astron. 30, 501.Google Scholar
Budding, E. 1984, Bull. Info. CDS. No. 27.Google Scholar
De Greve, J.P. and Cugier, 1989, Astron. Ap. 211, 356.Google Scholar
Giuricin, G., Mardirossian, F. and Mezzetti, M. 1983, Ap. J. Suppl. 52, 35.Google Scholar
Iben, I. 1967, Ann. Rev. Astron. Ap. 5, 571.Google Scholar
Iben, I. 1974, Ann. Rev. Astron. Ap. 12, 215.CrossRefGoogle Scholar
Kraicheva, Z.T. 1987, Nauchn. Informatssi, 63, 105.Google Scholar
Lambert, D.L. 1979, M.N.R.A.S. 182, 249.Google Scholar
Lambert, D.L. and Ries, L.M. 1981, Ap. J. 248, 228.Google Scholar
Parthasarathy, M., Lambert, D.L. and Tomkin, J. 1983, M.N.R.A.S. 203, 1063.Google Scholar
Yoon, T.S. 1991, Ph.D. dissertation, Indiana University Google Scholar