The orbital period of V458 Vulpeculae, a post-double common-envelope nova

P. Rodriguez-Gil, M. Santander-Garcia, C. Knigge, R.L.M. Corradi, B.T. Gansicke, M.J. Barlow, J. Drake, J.E. Drew, B. Miszalski, R. Napiwotzki, D. Steeghs, R. Wesson, A.A. Zijlstra, D.H. Jones, T. Liimets, T. Munoz-Darias, S. Pyrzas, M. Rubio-Diez

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Abstract

We present time-resolved optical spectroscopy of V458 Vulpeculae (Nova Vul 2007 No. 1) spread over a period of 15 months starting 301 d after its discovery. Our data reveal radial-velocity variations in the He II lambda 5412 and He II lambda 4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.096 47 +/- 0.000 25 min (0.068 122 55 +/- 0.000 000 17 d) which we identify with the orbital period of the binary system. V458 Vul is therefore the planetary nebula central binary star with the shortest period known. We explore the possibility of the system being composed of a relatively massive white dwarf (M-1 greater than or similar to 1.0 M-circle dot) accreting matter from a post-asymptotic giant branch star which produced the planetary nebula observed. In this scenario, the central binary system therefore underwent two common-envelope episodes. A combination of previous photoionization modelling of the nebular spectra, post-asymptotic gi! ant branch evolutionary tracks and the orbital period favour amass of M-2 similar to 0.6 M-circle dot for the donor star. Therefore, the total mass of the system may exceed the Chandrasekhar mass, which makes V458 Vul a Type Ia supernova progenitor candidate.
Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Volume407
Issue number1
DOIs
Publication statusPublished - 2010

Keywords

  • accretion
  • accretion discs
  • binaries : close
  • stars : individual : V458 Vul
  • novae
  • cataclysmic variables

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