Main-Sequence Stellar Eruption Model for V838 Monocerotis

Soker, Noam; Tylenda, R.

doi:10.1086/367759

Cited by 163 publications

(193 citation statements)

References 14 publications

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“…The cause of the outburst in these objects does not appear to be satisfactorily explained by conventional mechanisms. Thus, new theories have been proposed, viz., a scenario involving the merger of main-sequence stars (Soker & Tylenda 2003) and a hypothesis invoking planetary capture by an expanding star to explain the eruption (Retter & Marom 2003). The present data indicate that the second mechanism could be viable in V4332 Sgr.…”

mentioning

confidence: 54%

L and M Band Infrared Studies of V4332 Sagittarii: Detection of the Water Ice Absorption Band at 3.05 μm and the CO Fundamental Band in Emission

Banerjee

Varricatt²,

Ashok

2004

ApJ

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L and M band observations of the nova-like variable V4332 Sgr are presented. Two significant results are obtained, viz., the unusual detection of water ice at 3.05 mm and the fundamental band of 12 CO at 4.67 mm in emission. The ice feature is a first detection in a nova-like variable, while the CO emission is rarely seen in novae. These results, when considered together with other existing data, imply that V4332 Sgr could be a young object surrounded by a circumstellar disk containing gas, dust, and ice. The reason for a nova-like outburst to occur in such a system is unclear. But since planets are believed to form in such disks, it appears plausible that the enigmatic outburst of V4332 Sgr could be due to a planetary infall. We also give a more reliable estimate for an epoch of dust formation around V4332 Sgr that appears to have taken place rather late in 1999-nearly 5 years after its outburst.

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confidence: 54%

L and M Band Infrared Studies of V4332 Sagittarii: Detection of the Water Ice Absorption Band at 3.05 μm and the CO Fundamental Band in Emission

Banerjee

Varricatt²,

Ashok

2004

ApJ

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“…V383 Mon's behavior has so far eluded explanation or parallel. Soker & Tylenda (2003) proposed a stellar merging event (see also Kato 2003), but this would seem untenable in view of the apparent recurrent ejection episodes evidenced by the HST imagery (Bond et al 2003). The similarities between V838 Mon's behavior and that of M31 RV (Rich et al 1989), V4334 Sgr (Evans, Smalley, & Kimeswenger 2002), and V4332 Sgr (Martini et al 1999) have been noted by several groups (Wagner et al 2002b;Kimeswenger et al 2002;Munari et al 2002b;Bond et al 2003).…”

Section: Introductionmentioning

confidence: 88%

0.8–13 Micron Spectroscopy of V838 Monocerotis and a Model for Its Emission

Lynch

Rudy

Russell

et al. 2004

ApJ

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We report on the results of a number of infrared spectra (0.8-2.5, 2.1-4.6, and 3-14 m) of V838 Monocerotis, taken from a short time after discovery in 2002 January to about 14 months later, in early 2003. The spectrum evolved dramatically, changing from a quasi-photospheric stellar spectrum with weak atomic emission lines (some with P Cygni profiles) to one showing a wide range of deep absorption features indicative of a cool, extended atmosphere with a circumstellar dust shell. The early spectra showed lines of s-process elements, such as Sr ii and Ba i. The later spectra showed absorption by gaseous H 2 O, CO, AlO, TiO, SiO, SO 2 , OH, VO, and SH, as well as a complex of emission near 10 m reminiscent of silicate emission, with a central absorbing feature at 10:3 m. Thus, V838 Mon appears to be oxygen-rich. A simple, spherically symmetric model of the system involving a central star with a two-component expanding circumstellar shell is presented that is able to explain the major molecular features and spectral energy distribution in the object's late stages. The derived shell mass and distance are 0.04 M and 9.2 kpc, respectively.

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“…The most promising model appears to be that of a stellar collision followed by a merger (Soker & Tylenda 2003;Tylenda & Soker 2006). A crucial point in establishing the nature of the outburst is to constrain the evolutionary status of the progenitor of V838 Mon.…”

Section: Introductionmentioning

confidence: 99%

A molecular cloud within the light echo of V838 Monocerotis

Kamiński

Tylenda

Deguchi

2011

A&A

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Context. V838 Mon is an eruptive variable, which exploded in 2002. It displayed the most spectacular light echo ever observed. However, neither the origin of the reflecting matter nor the nature of the 2002 outburst have been firmly constrained. Aims. We investigate the nature of the CO radio emission detected in the field of the light echo. In particular, we explore its connection to the echoing dust around V838 Mon. Methods. We observed the echo region in multiple CO rotational transitions. We present and analyse maps of the region obtained in the 12 CO(1-0) and (3-2) lines. In addition, deep spectra at several positions were acquired in 12 CO(1-0), (2-1), (3-2), and 13 CO(1-0), (2-1). Radiative transfer modelling of line intensities is performed for chosen positions to constrain the kinetic temperatures and densities. We derive global parameters (e.g. mass, distance, total column density) of the emitting cloud. Results. We found that a compact molecular cloud is located within the echo region. The molecular emission is physically connected to the dusty environment seen in the optical echo and they both belong to the same translucent cloud. The interstellar nature of the cloud is confirmed by its high mass of 90-150 M . We propose that the cloud consists of material remaining after the formation of the cluster to which V838 Mon belongs. This indicates that the eruptive star has a young age (3-10 Myr).

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Main-Sequence Stellar Eruption Model for V838 Monocerotis

Cited by 163 publications

References 14 publications

L and M Band Infrared Studies of V4332 Sagittarii: Detection of the Water Ice Absorption Band at 3.05 μm and the CO Fundamental Band in Emission

L and M Band Infrared Studies of V4332 Sagittarii: Detection of the Water Ice Absorption Band at 3.05 μm and the CO Fundamental Band in Emission

0.8–13 Micron Spectroscopy of V838 Monocerotis and a Model for Its Emission

A molecular cloud within the light echo of V838 Monocerotis

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