Nova sagittarii 1998 (V4633 Sgr): A permanent superhump system or an asynchronous polar?

Y. Lipkin*, E. M. Leibowitz, A. Retter, O. Shemmer

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

17 Scopus citations

Abstract

We report the results of observations of V4633 Sgr (Nova Sagittarii 1998) during 1998-2000. Two photometric periodicities were present in the light curve during the three years of observations: a stable one at P = 3.014 h, which is probably the orbital period of the underlying binary system; and a second one of lower coherence, approximately 2.5 per cent longer than the former. The latter periodicity may be a permanent superhump, or, alternatively, the spin period of the white dwarf in a nearly synchronous magnetic system. A third period, at P = 5.06d, corresponding to the beat between the two periods was probably present in 1999. Our results suggest that a process of mass transfer has taken place in the binary system since no later than two-and-a-half months after the nova eruption. We derive an interstellar reddening of E(B - V) ∼ 0.21 from our spectroscopic measurements and published photometric data, and estimate a distance of d ~∼ 9 kpc to this nova.

Original languageEnglish
Pages (from-to)1169-1180
Number of pages12
JournalMonthly Notices of the Royal Astronomical Society
Volume328
Issue number4
DOIs
StatePublished - 21 Dec 2001

Keywords

  • Accretion, accretion discs-stars
  • Individual
  • V4633 Sgr-novae, cataclysmic variables

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