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Stellar chronology with white dwarfs in wide binaries

Published online by Cambridge University Press:  01 October 2008

S. Catalán ,
A. Garcés ,
I. Ribas ,
J. Isern  and
E. García-Berro
S. Catalán
Affiliation:
Institut d'Estudis Espacials de Catalunya, c/ Gran Capità 2–4, 08034 Barcelona, Spain email: catalan@ieec.uab.es Institut de Ciències de l'Espai, CSIC, Facultat de Ciències, UAB, 08193 Bellaterra, Spain
A. Garcés
Affiliation:
Institut d'Estudis Espacials de Catalunya, c/ Gran Capità 2–4, 08034 Barcelona, Spain email: catalan@ieec.uab.es Institut de Ciències de l'Espai, CSIC, Facultat de Ciències, UAB, 08193 Bellaterra, Spain
I. Ribas
Affiliation:
Institut d'Estudis Espacials de Catalunya, c/ Gran Capità 2–4, 08034 Barcelona, Spain email: catalan@ieec.uab.es Institut de Ciències de l'Espai, CSIC, Facultat de Ciències, UAB, 08193 Bellaterra, Spain
J. Isern
Affiliation:
Institut d'Estudis Espacials de Catalunya, c/ Gran Capità 2–4, 08034 Barcelona, Spain email: catalan@ieec.uab.es Institut de Ciències de l'Espai, CSIC, Facultat de Ciències, UAB, 08193 Bellaterra, Spain
E. García-Berro
Affiliation:
Institut d'Estudis Espacials de Catalunya, c/ Gran Capità 2–4, 08034 Barcelona, Spain email: catalan@ieec.uab.es Departament de Física Aplicada, Escola Politècnica Superior de Castelldefels, Universitat Politècnica de Catalunya, Avda. del Canal Olímpic s/n, 08860 Castelldefels, Spain
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Abstract

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White dwarfs are the evolutionary end product of stars with low and intermediate masses. The evolution of white dwarfs can be understood as a cooling process, which is relatively well known at the moment. For this reason, wide binaries containing white dwarfs are a powerful tool to constrain stellar ages. We have studied several wide binaries containing white dwarfs with two different purposes: when the age of the companion of the white dwarf can be determined with accuracy, we use the binary to improve the knowledge about the white dwarf member. On the contrary, if the companion is a low-mass star with no age indicator available, the white dwarf member itself is used to calibrate the age of the system. In this contribution we present some results using both methodologies to constrain the ages of wide binaries.

Keywords

stars: low-massstars: white dwarfsstars: binaries: visualstars: activitystars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S258: The Ages of Stars , October 2008 , pp. 307 - 314
Copyright
Copyright © International Astronomical Union 2009

References

Barnes, S. A. 2007, ApJ, 669, 1167Google Scholar
Bergeron, P., Wesemael, F., & Fontaine, G. 1992, ApJ, 387, 288Google Scholar
Catalán, S., Isern, J., García–Berro, E. et al. , 2008a, A&A, 477, 213Google Scholar
Catalán, S., Isern, J., García–Berro, E., & Ribas, I. 2008b, MNRAS, 387, 1693Google Scholar
Chanamé, J. & Gould, A. 2004, ApJ,601, 289Google Scholar
Domínguez, I., Chieffi, A., Limongi, M., & Straniero, O. 1999, ApJ, 524, 226CrossRefGoogle Scholar
Famaey, B., Jorissen, A., Luri, X. et al. , 2005, ESASP, 576, 129Google Scholar
Ferrario, L., Wickramasinghe, D. T., Liebert, J., & Williams, K. A. 2005, MNRAS, 361, 1131Google Scholar
Messina, S., Rodono, M., & Guinan, E. F. 2001, A&A, 366, 215Google Scholar
Isern, J., García-Berro, E., Hernanz, M., Mochkovitch, R., & Torres, S. 1998, ApJ, 503, 239Google Scholar
Kalirai, J. S., Hansen, M. S. B., Kelson, D. D. et al. , 2008, ApJ, 676, 594CrossRefGoogle Scholar
Kepler, S. O., Kleinman, S. J., Nitta, A. et al. , 2007, MNRAS, 375, 1315Google Scholar
Liebert, J., Young, P. A., Arnett, D., Holberg, J. B., & Williams, K. A. 2005, ApJ, 630, L69Google Scholar
Mamajek, E. E. & Hillenbrand, L. A. 2008, ApJ, 687, 1264Google Scholar
Montes, D., Fernandez-Figueroa, M. J., Cornide, M., & de Castro, E. 1996, ASPC, 109, 657Google Scholar
Oswalt, T. 1981, Ph. D. thesis, AA (Ohio State Univ., Columbus)Google Scholar
Oswalt, T., Hintzen, P., & Luyten, W. 1988, ApJS, 66, 391Google Scholar
Ribas, I., Guinan, E. F., Güdel, M., & Audard, M. 2005, ApJ, 622, 680Google Scholar
Salaris, M., García-Berro, E., Hernanz, M., Isern, J., & Saumon, D. 2000, ApJ, 544, 1036Google Scholar
Scalo, J., Kaltenegger, L., Segura, A. et al. 2007, AsBio, 7, 85Google Scholar
Silvestri, N. M., Hawley, S. L., & Oswalt, T. D. 2005, AJ, 129, 2428Google Scholar
Wegner, G. 1973, MNRAS, 165, 271Google Scholar
Weidemann, V. 2000, A&A, 363, 647Google Scholar
Williams, K. A. 2007, ASPCS, 372, 85Google Scholar