Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-23T08:44:52.352Z Has data issue: false hasContentIssue false
  • English
  • Français

V479 And: CV, LMXB, or Symbiotic?

Published online by Cambridge University Press:  17 January 2013

Diego González Buitrago ,
Gagik Tovmassian ,
Juan Echevarría ,
Sergey Zharikov ,
Takamitsu Miyaji ,
Andres Avilés  and
Gennady Valyavin
Diego González Buitrago
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 877, Ensenada, BC, 22800 Mexico
Gagik Tovmassian
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 877, Ensenada, BC, 22800 Mexico
Juan Echevarría
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 877, Ensenada, BC, 22800 Mexico
Sergey Zharikov
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 877, Ensenada, BC, 22800 Mexico
Takamitsu Miyaji
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 877, Ensenada, BC, 22800 Mexico
Andres Avilés
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 877, Ensenada, BC, 22800 Mexico
Gennady Valyavin
Affiliation:
Instituto de Astronomía, UNAM, Apdo. Postal 877, Ensenada, BC, 22800 Mexico
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.

V479 And is a 14.26 hour, close binary system, comprised of a G8-K0 star departing from the main sequence and a compact primary star accreting matter from the donor. The object is an X-ray source, modulated with the orbital period. This, and the presence of an intense He II line, leads us to speculate that the compact object is a magnetic white dwarf. However, we do not find strong constraints on the upper mass limit of the compact object, and we may have a neutron star in a low mass X-ray binary instead of a cataclysmic variable. The orbital period is certainly too short for the donor star to be an evolved giant star, so classifying this object as a symbiotic binary may be a big stretch; however there is an evidence that the mass transfer occurs via stellar winds, rather than through the L1 point of Roche filling secondary, a phenomenon more common for symbiotic stars.

Keywords

binaries: closespectroscopicsymbiotic — stars: novaecataclysmic variablesmagnetic fieldsindividual (V479 And, SDSS J001856.93+345444.3) — X-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 113 - 116
Copyright
Copyright © International Astronomical Union 2013

References

Bertelli, G., Girardi, L., Marigo, P., & Nasi, E. 2008, A&A, 484, 815Google Scholar
Campbell, R. K., Harrison, T. E., Schwope, A. D., & Howell, S. B. 2008, ApJ, 672, 531CrossRefGoogle Scholar
Dillon, M., et al. 2008, MNRAS, 386, 1568CrossRefGoogle Scholar
Echevarria, J. 1983, RevMexAA, 8, 109Google Scholar
Echevarría, J., Michel, R., Costero, R., & Zharikov, S. 2007, A&Ap, 462, 1069Google Scholar
Frank, J., Lasota, J.-P., & Chanmugam, G. 1995, ApJ, 453, 446Google Scholar
González, D., Tovmassian, G., Zharikov, S., Avilés, A., & Echevarria, J. 2010, arXiv:1009.5803Google Scholar
Knigge, C., Baraffe, I., & Patterson, J. 2011, ApJ (Supp.), 194, 28Google Scholar
McClintock, J. E., et al. 2003, ApJ, 593, 435CrossRefGoogle Scholar
Narayan, R., McClintock, J. E., & Yi, I. 1996, ApJ, 457, 821Google Scholar
Schwope, A. D., Mantel, K.-H., & Horne, K. 1997, A&Ap, 319, 894Google Scholar
Szkody, P., et al. 2005, AJ, 129, 2386Google Scholar
Szkody, P., et al. 2006, ApJ (Letters), 646, L147CrossRefGoogle Scholar