2011
DOI: 10.1051/0004-6361/201116865
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Connecting RS Ophiuchi to [some] type Ia supernovae

Abstract: Aims. Recurrent nova systems like RS Oph have been proposed as a possible channel for type Ia supernova (SN) explosions based on the high mass of the accreting white dwarf. Additional support for this hypothesis has recently been provided by the detection of circumstellar material around SN 2006X and SN 2007le, showing a structure compatible with that expected for recurrent nova outbursts. We investigate the circumstellar environment of RS Oph and its structure with the aim of establishing a firmer and indepen… Show more

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Cited by 84 publications
(97 citation statements)
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“…In the few SNe where time-variable Na ID is observed, the absorbing material appears consistent with nova shells which have plowed into and swept up a red giant wind (Wood-Vasey & Sokoloski 2006;Patat et al 2011), or an old nova shell expanding into the interstellar medium and decelerating (Moore & Bildsten 2012;Shen et al 2013). In the case of SN 2006X, the first SNIa to show time-variable absorption, deep radio limits were observed with the pre-upgrade VLA in the months following explosion, which should further constrain the radial distribution of material around the SN (Patat et al 2007;Chugai 2008).…”
Section: Na Id Absorption Featuresmentioning
confidence: 67%
“…In the few SNe where time-variable Na ID is observed, the absorbing material appears consistent with nova shells which have plowed into and swept up a red giant wind (Wood-Vasey & Sokoloski 2006;Patat et al 2011), or an old nova shell expanding into the interstellar medium and decelerating (Moore & Bildsten 2012;Shen et al 2013). In the case of SN 2006X, the first SNIa to show time-variable absorption, deep radio limits were observed with the pre-upgrade VLA in the months following explosion, which should further constrain the radial distribution of material around the SN (Patat et al 2007;Chugai 2008).…”
Section: Na Id Absorption Featuresmentioning
confidence: 67%
“…In symbiotic systems the wind from the giant companion star dominates the mass loss, with typical ratesṀ = 5×10 −9 to 5× 10 −6 M yr −1 and wind velocities v w < 100 km s −1 (Seaquist & Taylor 1990;Patat et al 2011;Chen et al 2011). Our limit on the environment density around SN 2014J strongly argues against this progenitor scenario (Figure 4).…”
Section: Sd With Quasi-steady Mass Lossmentioning
confidence: 71%
“…In the first scenario (single degenerate, SD, hereafter), the WD accretes material from the companion, potentially a giant, subgiant or main-sequence star (Whelan & Iben 1973;Hillebrandt & Niemeyer 2000;Nomoto 1982b). Wind from the secondary star provides material to be accreted (symbiotic channel; see, e.g., Patat et al 2011). Mass can be transferred to the WD via Roche lobe overflow (RLOF) from a hydrogen-rich mass-donor star or He star (Nomoto 1982a;van den Heuvel et al 1992;Iben & Tutukov 1994;Yoon & Langer 2003).…”
Section: Introductionmentioning
confidence: 99%
“…The asymmetric nature of such outflows could introduce a viewing angle dependence that would explain the apparent rarity of SNe Ia with variable Na I D. An alternative explanation, invoking variable line-of-sight absorption by ISM material far from the SN (Chugai 2008), explains the non-variability of the Ca II lines through abundance effects, by means of differing fractions of Ca and Na locked in dust grains in intervening clouds. Patat et al (2011) have noted the similarities of these variable absorptions with post-outburst features in the recurrent nova RS Ophiuchi (see Section 3.1.1, above). On the other hand, U Sco did not show any variable absorption during its outburst in 2010 (Kafka & Williams 2011).…”
Section: Intervening Absorptionmentioning
confidence: 81%