Four states of the recurrent symbiotic nova V407 Cyg

Есипов, В. Ф.; Kolotilov, E. A.; Комиссарова, Г. В.; Шенаврин, В. И.; Shugarov, S. Yu.; Тарасова, Т. Н.; Татарников, А. М.; Tatarnikova, A. A.

doi:10.1002/asna.201311927

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“…V407 Cyg has undergone periods of increased activity throughout the past several decades, observed as peaks in the optical light curve and brightening emission lines, particularly in the years 1936 and 1998 (Hoffmeister 1949;Welin 1973;Munari et al 1990;Kolotilov et al 1998Kolotilov et al , 2003Tatarnikova et al 2003a;Esipov et al 2012). These outbursts likely mark an increase in the accretion rate onto the WD (Kolotilov et al 2003), and so do not qualify as bona fide novae, which are powered by a thermonuclear runaway.…”

Section: Introductionmentioning

confidence: 99%

The Radio Light Curve of the Gamma-Ray Nova in V407 Cyg: Thermal Emission From the Ionized Symbiotic Envelope, Devoured From Within by the Nova Blast

Chomiuk

Krauss

Rupen

et al. 2012

ApJ

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We present multi-frequency radio observations of the 2010 nova event in the symbiotic binary V407 Cygni, obtained with the Karl G. Jansky Very Large Array (VLA) and spanning 1-45 GHz and 17-770 days following discovery. This nova-the first ever detected in gamma rays-shows a radio light curve dominated by the wind of the Mira giant companion, rather than the nova ejecta themselves. The radio luminosity grew as the wind became increasingly ionized by the nova outburst, and faded as the wind was violently heated from within by the nova shock. This study marks the first time that this physical mechanism has been shown to dominate the radio light curve of an astrophysical transient. We do not observe a thermal signature from the nova ejecta or synchrotron emission from the shock, due to the fact that these components were hidden behind the absorbing screen of the Mira wind. We estimate a mass-loss rate for the Mira wind ofṀ w ≈ 10 −6 M yr −1 . We also present the only radio detection of V407 Cyg before the 2010 nova, gleaned from unpublished 1993 archival VLA data, which shows that the radio luminosity of the Mira wind varies by a factor of 20 even in quiescence. Although V407 Cyg likely hosts a massive accreting white dwarf, making it a candidate progenitor system for a Type Ia supernova, the dense and radially continuous circumbinary material surrounding V407 Cyg is inconsistent with observational constraints on the environments of most Type Ia supernovae.

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