A nova-like red variable in M31

Mould, Jeremy; Cohen, Judith G.; Graham, James R.; Hamilton, Don; Matthews, K.; Picard, A.; Reid, Neill; Schmidt, Maarten; Soifer, Tom; Wilson, C. D.; Rich, R. Michael; Gunn, J. B.

doi:10.1086/185702

Cited by 78 publications

(101 citation statements)

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“…However, we believe that the standard deviation of an individual m v estimate is similar to that for an m B estimate. Our m v observations are useful to show that RV was a very red object in agreement with observations presented by Rich et al (1989) and Mould et al (1990).…”

Section: Magnitude Systemsupporting

confidence: 90%

Photometry of the unique luminous red variable in M31

Bryan¹,

Royer²

1992

PASP

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Section: Magnitude Systemsupporting

confidence: 90%

Photometry of the unique luminous red variable in M31

Bryan¹,

Royer²

1992

PASP

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“…Apart form V838 Mon, in our Galaxy the class also includes V4332 Sgr, whose outburst was observed in 1994 (Martini et al 1999), and V1309 Sco, which erupted in 2008 (Mason et al 2010). As extragalactic eruptions of this kind one can mention M 31 RV (eruption in 1989, Mould et al 1990), M 85 OT2006 (Kulkarni et al 2007), and NGC300 OT2008 (Berger et al 2009). Several interpretations of the eruptions were proposed.…”

Section: Introductionmentioning

confidence: 91%

V1309 Scorpii: merger of a contact binary

Tylenda

Hajduk

Kamiński

et al. 2011

A&A

440

611

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Context. Stellar mergers are expected to take place in numerous circumstences in the evolution of stellar systems. In particular, they are considered as a plausible origin of stellar eruptions of the V838 Mon type. V1309 Sco is the most recent eruption of this type in our Galaxy. The object was discovered in September 2008. Aims. Our aim is to investigate the nature of V1309 Sco. Methods. V1309 Sco has been photometrically observed in course of the OGLE project since August 2001. We analyse these observations in different ways. In particular, periodogram analyses were done to investigate the nature of the observed short-term variability of the progenitor. Results. We find that the progenitor of V1309 Sco was a contact binary with an orbital period of ∼1.4 day. This period was decreasing with time. The light curve of the binary was also evolving, indicating that the system evolved towards its merger. The violent phase of the merger, marked by the systematic brightenning of the object, began in March 2008, i.e. half a year before the outburst discovery. We also investigate the observations of V1309 Sco during the outburst and the decline and show that they can be fully accounted for within the merger hypothesis. Conclusions. For the first time in the literature we show from direct observations that contact binaries indeed end up by merging into a single object, as was suggested in numerous theoretical studies of these systems. Our study also shows that stellar mergers indeed result in eruptions of the V838 Mon type.

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“…(2007)) to have physical properties inconsistent with all of the nova models in Paper I. While thermonuclear-powered nova eruptions can explain the luminosities of these objects, their massive and very cool ejecta seem totally different from those of other novae (Mould et al (1990), Bond et al (2003), Munari et al (2002), Banerjee & Ashok (2002), Kimeswenger et al (2002), Soker & Tylenda (2003), Kipper, Klochkova, & Annuk (2004), Lynch et al (2004)). Does the nova model fail for these objects?…”

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confidence: 86%

An Extended Grid of Nova Models. Iii. Very Luminous, Red Novae

Shara

Yaron

Prialnik

et al. 2010

ApJ

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Extremely luminous, red eruptive variables like RV in M31 are being suggested as exemplars of a new class of astrophysical object. Our greatly extended series of nova simulations shows that classical nova models can produce very red, luminous eruptions. In a poorly studied corner of 3-D nova parameter space (very cold, low-mass white dwarfs, accreting at very low rates) we find bona fide classical novae that are very luminous and red because they eject very slowly moving, massive envelopes. A crucial prediction of these nova models -in contrast to the predictions of merging star ("mergeburst") models -is that a hot remnant, the underlying white dwarf, will emerge after the massive ejected envelope has expanded enough to become optically thin. This blue remnant must fade on a timescale of decades -much faster than a "mergeburst", which must fade on timescales of millenia or longer. Furthermore, the cooling nova white dwarf and its expanding ejecta must become redder in the years after eruption, while a contracting mergeburst must become hotter and bluer. We predict that red novae will always brighten to L ∼ 1000L ⊙ for about 1 year before rising to maximum luminosity at L ∼ 10 6 − 10 7 L ⊙ . The maximum luminosity attainable by a nova is likely to be L ∼ 10 7 L ⊙ , corresponding to M ∼ −12. In an accompanying paper we describe a fading, luminous blue candidate for the remnant of M31-RV; it is observed with HST to be compatible only with the nova model.

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A nova-like red variable in M31

Cited by 78 publications

References 1 publication

Photometry of the unique luminous red variable in M31

Photometry of the unique luminous red variable in M31

V1309 Scorpii: merger of a contact binary

An Extended Grid of Nova Models. Iii. Very Luminous, Red Novae

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