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

研究成果: Article査読

10 被引用数 (Scopus)

抄録

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.

本文言語English
ページ(範囲)68-75
ページ数8
ジャーナルBaltic Astronomy
21
1-2
DOI
出版ステータスPublished - 2012

ASJC Scopus subject areas

  • 天文学と天体物理学
  • 宇宙惑星科学

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