<i>Hubble Space Telescope</i>Imaging of the Outburst Site of M31 RV

Bond, Howard E.; Siegel, M. H.

doi:10.1086/498896

Cited by 30 publications

(32 citation statements)

References 29 publications

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“…Kato (2003) suggests that Nova CK Vul 1670 might have been a stellar merger event. Bond & Siegel (2005) mention that Nova V1148 Sgr 1943 had a late-type spectrum thus being a possible object of the V838 Mon type. It is quite probable that some V838 Mon type objects remain hidden among stars catalogued as classical nova or nova-like.…”

Section: Summary and Discussionmentioning

confidence: 98%

Eruptions of the V838 Mon type: stellar merger versus nuclear outburst models

Tylenda

Soker

2006

A&A

145

153

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We discuss various models and scenarios proposed to explain the nature of the V838 Mon type eruptions. In this class of eruptive objects we include: M 31 RV (erupted in 1988), V4332 Sgr (erupted in 1994) and V838 Mon (erupted in 2002). We concentrate on three models: (i) thermonuclear runaway on an accreting white dwarf (nova-like event); (ii) He-shell flash in a post asymptotic giant branch star (born-again AGB); and (iii) merger of stars. We show that models (i) and (ii) cannot account for the majority of the observed properties of the objects. Most significantly, in both nuclear burning type models the object is expected to heat up before declining and fade as a very hot compact star. In the observed eruptions the objects declined as very cool giants or supergiants. We show that the stellar merger model can account for all the observed properties and conclude that presently this is the most promising model to explain the eruptions of the V838 Mon type.

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Section: Summary and Discussionmentioning

confidence: 98%

Eruptions of the V838 Mon type: stellar merger versus nuclear outburst models

Tylenda

Soker

2006

A&A

145

153

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“…Bond & Siegel (2006) examined the site of the eruption in Hubble Space Telescope images and reported that "there is no evidence for any significant young population at this location in the M31 bulge". M85-OT erupted near the lenticular galaxy (Hubble type S0) M85.…”

Section: Stellar Populationsmentioning

confidence: 99%

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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“…This is because they are restricted to a single type of stars, while the members in the V838 Mon class are of different kinds. It was concluded that the progenitor of V838 Mon is a B supergiant while that of V4332 Sgr, and most likely M31RV, are red giants (Tylenda et al 2005a; Bond & Siegel 2006). Therefore, only scenarios that use different types of stars could be invoked to explain their eruptions.…”

Section: Discussionmentioning

confidence: 99%

“…Soon after its outburst, V838 Mon was recognized as the prototype of a new class of stars (Munari et al 2002; Bond et al 2003), which currently consists of three objects: 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 V838 Mon (Peculiar Red Variable in 2002), plus three candidates – CK Vul, which was identified with an object that had a nova‐like event in the year 1670 (Shara & Moffat 1982; Shara, Moffat & Webbink 1985; Kato 2003; Retter & Marom 2003), V1148 Sgr, which had a nova outburst in 1943 and was reported to have a late‐type spectrum (Mayall 1949; Bond & Siegel 2006) and the peculiar variable in Crux that erupted in 2003 (Della Valle et al 2003).…”

Section: Introductionmentioning

confidence: 99%

The planets capture model of V838 Monocerotis: conclusions for the penetration depth of the planet(s)

Retter

Zhang

Siess

et al. 2006

Monthly Notices of the Royal Astronomical Society

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V838 Mon is the prototype of a new class of objects. Understanding the nature of its multistage outburst and similar systems is challenging. So far, several scenarios have been invoked to explain this group of stars. In this work, the planets‐swallowing model for V838 Mon is further investigated, taking into account the findings that the progenitor is most likely a massive B‐type star. We find that the super‐Eddington luminosity during the eruption can explain the fast rising times of the three peaks in the optical light curve. We used two different methods to estimate the location where the planets were consumed. There is a nice agreement between the values obtained from the luminosities of the peaks and from their rising time‐scale. We estimate that the planets were stopped at a typical distance of one solar radius from the centre of the host giant star. The planets‐devouring model seems to give a satisfying explanation to the differences in the luminosities and rising times of the three peaks in the optical light curve of V838 Mon. The peaks may be explained by the consumption of three planets or alternatively by three steps in the terminal falling process of a single planet. We argue that only the binary merger and the planets‐swallowing models are consistent with the observations of the new type of stars defined by V838 Mon.

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Hubble Space TelescopeImaging of the Outburst Site of M31 RV

Cited by 30 publications

References 29 publications

Eruptions of the V838 Mon type: stellar merger versus nuclear outburst models

Eruptions of the V838 Mon type: stellar merger versus nuclear outburst models

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

The planets capture model of V838 Monocerotis: conclusions for the penetration depth of the planet(s)

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