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Open Astronomy

formerly Baltic Astronomy

Editor-in-Chief: Barbuy, Beatriz

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Volume 21, Issue 1-2


An Extremely Massive White Dwarf of the Symbiotic Classical Nova V407 Cyg as Suggested by the RS Oph and U SCO Models

I. Hachisu
  • Corresponding author
  • Department of Earth Science and Astronomy, College of Arts and Sciences, Uni. of Tokyo, Tokyo 153-8902, Japan
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ M. Kato
Published Online: 2017-03-23 | DOI: https://doi.org/10.1515/astro-2017-0360


We have analyzed the optical light curve of the symbiotic star V407 Cyg that underwent a classical nova outburst in 2010 March. Being guided by a supersoft X-ray phase observed during days 20-40 after the nova outburst, we are able to reproduce the light curve during a very early phase of the nova outburst. Our model consists of an outbursting white dwarf and an extended equatorial disk. An extremely massive white dwarf of 1.35-1.37 M is suggested. the optical light curve is also consistent with a sharp drop 47 days after the outburst, which is the end of hydrogen shell-burning on the white dwarf. Although the extremely massive white dwarf is favourable to the interpretation that V407 Cyg is a recurrent nova, enrichment of heavy elements in the ejecta suggests that the white dwarf is eroded and, as a result, its mass is not increasing. Therefore, V407 Cyg may not explode as a Type Ia supernova even if it is a carbon-oxygen white dwarf.

Keywords: binaries; symbiotic; novae; cataclysmic variables; stars; individual (RS Oph; U Sco; V407 Cyg); white dwarfs


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About the article

Received: 2011-09-01

Accepted: 2011-09-15

Published Online: 2017-03-23

Published in Print: 2012-06-01

Citation Information: Open Astronomy, Volume 21, Issue 1-2, Pages 68–75, ISSN (Online) 2543-6376, DOI: https://doi.org/10.1515/astro-2017-0360.

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© 2017. This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 License. BY-NC-ND 4.0

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