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Close binary evolution and blue straggler formation

Published online by Cambridge University Press:  01 April 2008

P. Lu.  and
L. Deng
P. Lu.
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P.R. China email: lupin@bao.ac.cn Graduate University of ChineseAcademy of Sciences, Beijing, 100049, P.R. China
L. Deng
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P.R. China email: lupin@bao.ac.cn
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Abstract

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In order to discuss the contribution of mass transfer in primordial close binaries to the blue straggler population in young clusters, we use Eggleton's stellar evolution code to simulate a grid of case A binary evolutionary models with the initial donor mass 2.0 – 8.0 M⊙ and mass ratio 0.1 – 0.9. The models cover the whole case A binaries that will experience mass transfer between 30.0 Myr to 1.0 Gyr. Based on such detailed models, we present a simulation to compare with the HST observation of young cluster NGC 1831 which can be fit with an isochrone of log(age) = 8.65. The results show very few blue stragglers could be produced by case A binary evolution. There must be some other mechanisms for blue straggler formation in young clusters.

Keywords

Stars: blue stragglersstars: binaries: closeGalaxy: open clusters and associations: individual (NGC 1831)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 371 - 377
Copyright
Copyright © International Astronomical Union 2008

References

Alexander, D. R. & Ferguson, J. W. 1994, ApJ 437, 879CrossRefGoogle Scholar
Chen, X. F. & Han, Z. W. 2004, MNRAS 355, 1182CrossRefGoogle Scholar
Deng, L., Chen, R., Liu, X. S., & Chen, J. S. 1999, ApJ 524, 824CrossRefGoogle Scholar
Eggleton, P. P. 1971, MNRAS 151, 351CrossRefGoogle Scholar
Eggleton, P. P. 1972, MNRAS 156, 361CrossRefGoogle Scholar
Eggleton, P. P. 1973, MNRAS 163, 279CrossRefGoogle Scholar
Han, Z., Podsiadlowski, Ph., & Eggleton, P. P. 1994, MNRAS 270, 121CrossRefGoogle Scholar
Han, Z., Tout, C. A., & Eggleton, P. P. 2000, MNRAS 319, 215CrossRefGoogle Scholar
Hurly, J. R., Tout, C. A., Aarseth, S. J., & Pols, O. R. 2001, MNRAS 323, 630CrossRefGoogle Scholar
Hurly, J. R., Pols, O. R., Aarseth, S. J., & Tout, C. A. 2001, MNRAS 363, 293CrossRefGoogle Scholar
Iglesias, C. A. & Rogers, F. J. 1996, ApJ 464, 943CrossRefGoogle Scholar
Kroupa, P., Tout, C. A., & Gilmore, G. 1991, MNRAS 251, 293CrossRefGoogle Scholar
Lejeune, Th., Cuisinier, F., & Buser, R. 1997, A&AS 125, 229Google Scholar
Lejeune, Th., Cuisinier, F., & Buser, R. 1998, A&AS 130, 65Google Scholar
McCrea, W. H. 1964, A&A 128, 147Google Scholar
Pols, O. R. & Marinus, M. 1994, A&A 288, 475Google Scholar
Pols, O. R., Tout, C. A., Eggleton, P. P., & Han, Z. 1995, MNRAS 274, 964CrossRefGoogle Scholar
Pols, O. R., Schroder, K.-P., Hurley, J. R., Tout, C. A., & Eggleton, P. P. 1998, MNRAS 298, 525CrossRefGoogle Scholar
Sandage, A. R. 1953, AJ 58, 61CrossRefGoogle Scholar
Tian, B., Deng, L., Han, Z., & Zhang, X. B. 2006, A&AS 455, 247Google Scholar
Xin, Y. & Deng, L. 2005, ApJ 619, 824CrossRefGoogle Scholar