Discovery of multiple shells around V838 Monocerotis

Loon, Jacco Th. van; Evans, A.; Rushton, M. T.; Smalley, B.

doi:10.1051/0004-6361:20041388

Cited by 16 publications

(32 citation statements)

References 13 publications

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“…3.2. The emission that van Loon et al (2004) plotted as the upper-left section of their CO loop comes from the survey of Dame et al (1987) and is way down in the noise of this survey.…”

Section: Discussion and Summarymentioning

confidence: 99%

“…van Loon et al (2004) argue that there are multiple shells around V838 Mon, which were ejected by V838 Mon in previous eruptions. Hence they reason that prior to eruption V838 Mon was an asymptotic giant branch (AGB) star.…”

Section: Introductionmentioning

confidence: 99%

“…van Loon et al (2004) have also analyzed the expansion of the light echo. Their analysis has been based on their measurements of the echo diameter on images from different sources.…”

Section: Introductionmentioning

confidence: 99%

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On the progenitor of V838 Monocerotis

Tylenda

Soker²,

Szczerba

2005

A&A

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We summarize and analyze the available observational data on the progenitor and the environment of V838 Mon. From the available photometric data for the progenitor of V838 Mon we exclude the possibility that the object before eruption was an evolved red giant star (AGB or RGB star). We find that most likely it was a main sequence or pre-main sequence star of ∼5−10 M . From the light echo structure and evolution we conclude that the reflecting dust is of interstellar nature rather than blown by V838 Mon in the past. We discuss the IRAS and CO data for interstellar medium observed near the position of V838 Mon. Several interstellar molecular regions have radial velocities similar to that of V838 Mon, so dust seen in the light echo might be related to one of them.

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“…3.2. The emission that van Loon et al (2004) plotted as the upper-left section of their CO loop comes from the survey of Dame et al (1987) and is way down in the noise of this survey.…”

Section: Discussion and Summarymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On the progenitor of V838 Monocerotis

Tylenda

Soker²,

Szczerba

2005

A&A

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“…(However there is no direct evidence that both components form a real binary.) The system is embedded in the interstellar medium, which is most likely to be related to molecular clouds seen around the position of V838 Mon, rather than to be expelled by the object itself as argued by van Loon et al (2004).…”

Section: Introductionmentioning

confidence: 98%

Evolution of V838 Monocerotis during and after the 2002 eruption

Tylenda

2005

A&A

166

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Abstract. By fitting the available photometric data on V838 Mon with standard supergiant spectra we have derived principal stellar parameters, i.e. effective temperature, radius and luminosity, and followed the evolution of the object since its discovery in early January 2002. Our analysis shows that the 2002 outburst of V838 Mon consisted of two major phases: pre-eruption, which was observed in January 2002 and a major outburst, the eruption, which started in the beginning of February 2002. During pre-eruption the object seemed to be relaxing after an initial event which had presumably taken place in last days of December 2001. The eruption phase, which lasted until mid-April 2002, resulted from a very strong energy burst, which presumably took place in last days of January at the base of the stellar envelope inflated in pre-eruption. The burst produced an energy wave, which was observed as a strong luminosity flash in the beginning of February, followed by a strong mass outflow in the form of two shells, which was observed as an expanding photosphere in later epochs. In mid-April, when the outflow became optically transparent and most of its energy radiated away, the object entered the decline phase during which V838 Mon was evolving along the Hayashi track. This we interpret as evidence that the main energy source during decline was gravitational contraction of the object envelope inflated in eruption. Late in 2002, dust formation started in the expanding shells which gave rise to a strong infrared excess observed in 2003.

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“…Another possibility is the merger of a pair of mainsequence binary stars (Soker & Tylenda 2003). It has also been suggested that V838 Mon is a post-asymptotic giant branch (AGB) star and the event was due to He flash (van Loon et al 2004). Finally, Retter & Marom (2003) have suggested that the eruption was due to the accretion of several close-in giant planets by an expanding giant or AGB star.…”

Section: Introductionmentioning

confidence: 99%

Interferometric Observations of V838 Monocerotis

Lane¹,

Retter²,

Thompson³

et al. 2005

ApJ

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We have used long-baseline near-IR interferometry to resolve the peculiar eruptive variable star V838 Mon and to provide the first direct measurement of its angular size. Assuming a uniform disk model for the emission, we derive an apparent angular diameter at the time of observations (2004 November-December) of 1.83 ‫ע‬ mas. For a nominal distance of kpc, this implies a linear radius of 1570 ‫ע‬ 400 R , . However, the 0.06 8 ‫ע‬ 2 data are somewhat better fitted by elliptical disk or binary component models, and we suggest that the emission may be strongly affected by ejecta from the outburst.

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Discovery of multiple shells around V838 Monocerotis

Cited by 16 publications

References 13 publications

On the progenitor of V838 Monocerotis

On the progenitor of V838 Monocerotis

Evolution of V838 Monocerotis during and after the 2002 eruption

Interferometric Observations of V838 Monocerotis

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