Photometry of the unique luminous red variable in M31

Bryan, J. T.; Royer, R.

doi:10.1086/132975

Cited by 19 publications

(21 citation statements)

References 10 publications

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“…The maximum observed brightnesses attained by M31 RV were V=15.3 (Bryan & Royer 1992) and I=14.9 (Rich et al 1989). The maximum absolute magnitude was thus at least M = −9.3, or 4 × 10 5 L ⊙ .…”

Section: M31 Rvmentioning

confidence: 86%

“…As pointed out by Rich et al (1989), at peak brightness M31-RV approached a bolometric magnitude M bol = −9.6, making it the most luminous red supergiant in the Local Group. The key observational constraints on this remarkable star have been presented by Rich et al (1989), Mould et al (1990), Bryan & Royer (1992), Tomaney & Shafter (1992), and Boschi & Munari (2004). These observed characteristics and constraints (summarized below) must be mimicked by any model that seeks to explain this and similar outbursts.…”

Section: M31 Rvmentioning

confidence: 96%

“…The time to brighten the last 3 or 4 magnitudes to maximum light was less than 29 days, and could have been as short as hours or a few days (Bryan & Royer 1992).…”

Section: M31 Rvmentioning

confidence: 99%

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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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Section: M31 Rvmentioning

confidence: 86%

Section: M31 Rvmentioning

confidence: 96%

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

Shara

Yaron

Prialnik

et al. 2010

ApJ

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“…A few other stars have shown several observational similarities to V838 Mon, and in particular similar colour evolution, but the observational data of these objects are relatively scarce. The list includes M31RV (Red Variable in M31 in 1988) (Rich et al 1989; Mould et al 1990; Bryan & Royer 1992), V4332 Sgr (Luminous Variable in Sgr, 1994) (Martini et al 1999) and maybe also CK Vul (Nova‐? Vul 1670) (Shara, Moffat & Webbink 1985; Kato 2003).…”

Section: Other Considerationsmentioning

confidence: 99%

A model of an expanding giant that swallowed planets for the eruption of V838 Monocerotis

Retter

Marom

2003

Monthly Notices RAS

102

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In early 2002 V838 Monocerotis had an extraordinary outburst, the nature of which is still unclear. The optical light curve showed at least three peaks, and imaging revealed a light echo around the object – evidence for a dust shell which was emitted several thousand years ago and now reflecting light from the eruption. Spectral analysis suggests that the object was relatively cold throughout the event, which was characterized by an expansion to extremely large radii. We show that the three peaks in the light curve have a similar shape and thus it seems likely that a certain phenomenon was three times repeated. Our suggestion that the outburst was caused by the expansion of a red giant, followed by the successive swallowing of three relatively massive planets in close orbits, supplies a simple explanation to all observed peculiarities of this intriguing object.

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“…In mid-1988, an unusual stellar outburst in the nuclear bulge of the Andromeda galaxy, M31, was discovered independently by Rich et al (1989), Bryan & Royer (1992), and Tomaney & Shafter (1992). Although similar in luminosity to a classical nova, the object was cool and red throughout its eruption.…”

Section: Introductionmentioning

confidence: 99%

Hubble Space TelescopeImaging of the Outburst Site of M31 RV

Bond

Siegel

2006

Astron J

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M31 RV is a luminous red variable star that appeared for several months in the bulge of M31 during 1988. Unlike classical novae, M31 RV was cool throughout its outburst. Interest in this object has been revived recently because of its strong resemblance to V838 Mon, a luminous Galactic variable star that appeared in 2002 and is illuminating a spectacular light echo, and has evolved to ever cooler surface temperatures. ( V4332 Sgr is a third object that was also a red supergiant throughout its eruption.) We have examined archival Hubble Space Telescope (HST ) images of the site of M31 RV, obtained fortuitously in 1999 with the WFPC2 camera in parallel mode during spectroscopic observations of the nucleus of M31. We located the site of M31 RV in the HST frames precisely through astrometric registration with ground-based CCD images, including several taken during the outburst. No light echo is seen at the M31 RV site, implying either that M31 RV is not surrounded by circumstellar (or interstellar) dust similar to that around V838 Mon, or that its extent is less than $1.7 pc. The stellar population at the outburst site consists purely of old red giants; there is no young population, such as that seen around V838 Mon. There are no stars of unusual color at the site, suggesting either that M31 RV had faded below HST detectability in the 11 years since outburst, that it is an unresolved companion of one of the red giants in the field, or that it is one of the red giants. We suggest future observations that may help decide among these possibilities.

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Photometry of the unique luminous red variable in M31

Abstract: ABSTRACT. We present additional photometric observations of an unusual red nova that appeared in M31 in 1988. Its luminosity was greater than that of a typical classical nova, and its decline was unusually slow.

Cited by 19 publications

References 10 publications

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

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

A model of an expanding giant that swallowed planets for the eruption of V838 Monocerotis

Hubble Space TelescopeImaging of the Outburst Site of M31 RV

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