On the progenitor of V838 Monocerotis

Tylenda, R.; Soker, Noam; Szczerba, R.

doi:10.1051/0004-6361:20042485

Cited by 52 publications

(100 citation statements)

References 36 publications

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“…For a fixed distance, the expansion of the echo outer rim is uniquely determined by z 0 . The observed expansion of the light echo outer rim, as measured in Tylenda et al (2005) and compared to the results of our modelling in Fig. 2, results in z 0 2.1 pc.…”

Section: The Modelsupporting

confidence: 79%

Light echo of V838 Monocerotis: properties of the echoing medium

Tylenda

Kamiński

2012

A&A

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Context. The light echo phenomenon that accompanied the 2002 eruption of V838 Mon allows one to study the properties of the diffuse dusty matter in the vicinity of the object. Aims. We are aiming at obtaining estimates of the optical thickness of the circumstellar matter in front of V838 Mon, as well as optical properties of dust grains in the echoing medium. In particular, we are interested in studying whether the echoing medium can be responsible for the observed faintness of the B-type companion of V838 Mon when compared to three B-type stars that are seen in the vicinty of V838 Mon and are believed to be at the same distance as V838 Mon. Methods. We used the V838 Mon light echo images obtained by the Hubble Space Telescope (HST) in different filters and epochs. From the images we derived the total brightness of the echo and its surface brightness. The results of the measurements were compared to model light echoes.Results. The present study allowed us to estimate the optical thickness of the matter in front of the object and the mean cosine value of the scattering angle of dust grains in three HST filters. Conclusions. The optical thickness of the echoing matter is not sufficient to explain the observed difference in brightness between the B-type companion of V838 Mon and the other three B-type stars observed in the vicinity of V838 Mon. Implications of this result are discussed. Our estimate of the mass of the diffuse matter seen in the light echo shows that the matter cannot have resulted from a past mass loss activity of V838 Mon. We probably observe remnants of an interstellar cloud from which V838 Mon and other members of the observed cluster were formed.

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Section: The Modelsupporting

confidence: 79%

Light echo of V838 Monocerotis: properties of the echoing medium

Tylenda

Kamiński

2012

A&A

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“…If V838 Mon and the B3 V companion are observed at the same position in the sky due to a random coincidence then, apart from the above possibilities, the progenitor of V838 Mon could have been either a BA-type giant of mass > ∼ 2.5 M or a B-type post-AGB star (Tylenda et al 2005b). In both cases a white dwarf companion cannot be excluded.…”

Section: Nova-like Outburstsmentioning

confidence: 97%

“…Gravitational contraction powers protostars. It is possible, as discussed in Tylenda et al (2005b), that the progenitor of V838 Mon was a pre-main-sequence star. However there is no known way in which an energy of > ∼ 3 × 10 46 erg s −1 could be released on a time scale of a month in a pre-main-sequence star.…”

Section: The Stellar Merger Modelmentioning

confidence: 97%

“…The object is surrounded by extended circumstellar matter seen in the light echo (Munari et al 2002b;Bond et al 2003). The matter is most likely of interstellar origin, possibly being part of one of the star forming regions seen in the direction of and at similar distances as V838 Mon (Tylenda 2004;Tylenda et al 2005b).…”

Section: Observed Propertiesmentioning

confidence: 99%

“…an ∼A0 spectral type discussed in Tylenda et al (2005b). The stellar radii were R 1 = 8 R and R 2 = 2 R .…”

Section: Numerical Simulationsmentioning

confidence: 99%

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

Tylenda

Soker

2006

A&A

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146

152

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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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Common envelope evolution: where we stand and how we can move forward

Іванова

Justham

Chen

et al. 2013

Astron Astrophys Rev

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922

587

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This work aims to present our current best physical understanding of common-envelope evolution (CEE). We highlight areas of consensus and disagree- ment, and stress ideas which should point the way forward for progress in this important but long-standing and largely unconquered problem. Unusually for CEE-related work, we mostly try to avoid relying on results from population synthesis or observations, in order to avoid potentially being misled by previous misunderstandings. As far as possible we debate all the relevant issues starting from physics alone, all the way from the evolution of the binary system immediately before CEE begins to the processes which might occur just after the ejection of the envelope. In particular, we include extensive discussion about the energy sources and sinks operating in CEE, and hence examine the foundations of the standard energy formalism. Special attention is also given to comparing the results of hydrodynamic simulations from different groups and to discussing the potential effect of initial conditions on the differences in the outcomes. We compare current numerical techniques for the problem of CEE and also whether more appropriate tools could and should be produced (including new formulations of computational hydrodynamics, and attempts to include 3D processes within 1D codes). Finally we explore new ways to link CEE with observations. We compare previous simulations of CEE to the recent outburst from V1309 Sco, and discuss to what extent post-common-envelope binaries and nebulae can provide information, e.g. from binary eccentricities, which is not currently being fully exploited.

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On the progenitor of V838 Monocerotis

Cited by 52 publications

References 36 publications

Light echo of V838 Monocerotis: properties of the echoing medium

Light echo of V838 Monocerotis: properties of the echoing medium

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

Common envelope evolution: where we stand and how we can move forward

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