Resumption of mass accretion in RS Oph

H. L. Worters, S. P. S. Eyres, G. E. Bromage, J. P. Osborne

Research output: Contribution to journalArticlepeer-review


The latest outburst of the recurrent nova RS Oph occurred in 2006 February. Photometric data presented here show evidence of the resumption of optical flickering, indicating re-establishment of accretion by day 241 of the outburst. Magnitude variations of up to 0.32 mag in V band and 0.14 mag in B band on time-scales of 600–7000 s are detected. Over the two-week observational period, we also detect a 0.5 mag decline in the mean brightness, from V≈ 11.4 to 11.9, and record B≈ 12.9 mag. Limits on the mass accretion rate of inline image are calculated, which span the range of accretion rates modelled for direct wind accretion and Roche lobe overflow mechanisms. The current accretion rates make it difficult for thermonuclear runaway models to explain the observed recurrence interval, and this implies average accretion rates are typically higher than seen immediately post-outburst.

Original languageEnglish
Pages (from-to)1557-1561
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
Publication statusPublished - 21 Aug 2007


  • binaries: symbiotic
  • Stars: individual: RS Oph
  • stars: mass-loss
  • novae, cataclysmic variables
  • stars: winds, outflows


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