An extremely massive white dwarf of the symbiotic classical nova V407 Cyg as suggested by the rs oph and u sco models

I. Hachisu, M. Kato

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8 Citations (Scopus)

Abstract

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.

Original languageEnglish
Pages (from-to)68-75
Number of pages8
JournalBaltic Astronomy
Volume21
Issue number1-2
Publication statusPublished - 2012 Jun 11

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Keywords

  • Binaries: Symbiotic
  • Novae, cataclysmic variables
  • Stars: Individual (rs oph, u sco, v407 cyg)
  • White dwarfs

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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