V838 Mon: an L supergiant?

Evans, A.; Geballe, T. R.; Rushton, M. T.; Smalley, B.; Loon, Jacco Th. van; Eyres, S. P. S.; Tyne, V. H.

doi:10.1046/j.1365-8711.2003.06755.x

Cited by 67 publications

(91 citation statements)

References 19 publications

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“…Finally, association of the OH with the outer photosphere enables the mass of the outer photosphere to be estimated, resulting in 0.008-0.03 M (it depends on the assumed area of the outer photosphere, 1 2A p ). This is in agreement with the estimates made by Evans et al (2003).…”

Section: Derived Quantitiessupporting

confidence: 94%

“…A few months after the outburst, V838 Mon was found to be part of a binary system, with the companion being a B3 V star (Desidera & Munari 2002;. Infrared observations interspersed with our own and covering the 1-2.5 m region have been reported by Evans et al (2003), who speculate that V838 Mon may be an L giant, an interesting possibility in view of the object's low temperature and pressure.…”

Section: Introductionmentioning

confidence: 60%

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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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Section: Derived Quantitiessupporting

confidence: 94%

Section: Introductionmentioning

confidence: 60%

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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“…colonel Roche, BP 44346, 31028 Toulouse, France spectral types F, G, and K, to a very cool M-giant (Evans et al 2003). Loebman et al (2015) found the star to show features of mixed spectral type, from M3 dwarf to mid-L supergiant: the atmosphere is obviously not a conformist.…”

Section: Post Outburst V838 Mon Varied Throughmentioning

confidence: 99%

On the properties of dust and gas in the environs of V838 Monocerotis

Exter

Cox

Swinyard

et al. 2016

A&A

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Aims. We aim to probe the close and distant circumstellar environments of the stellar outburst object V838 Mon. Methods. Herschel far-infrared imaging and spectroscopy were taken at several epochs to probe the central point source and the extended environment of V838 Mon. PACS and SPIRE maps were used to obtain photometry of the dust immediately around V838 Mon, and in the surrounding infrared-bright region. These maps were fitted in 1d and 2d to measure the temperature, mass, and β of the two dust sources. PACS and SPIRE spectra were used to detect emission lines from the extended atmosphere of the star, which were then modelled to study the physical conditions in the emitting material. HIFI spectra were taken to measure the kinematics of the extended atmosphere but unfortunately yielded no detections. Results. Fitting of the far-infrared imaging of V838 Mon reveals 0.5−0.6 M of ≈19 K dust in the environs (≈2.7 pc) surrounding V838 Mon. The surface-integrated infrared flux (signifying the thermal light echo), and derived dust properties do not vary significantly between the different epochs. We measured the photometry of the point source. As the peak of the SED (Spectral Energy Distribution) lies outside the Herschel spectral range, it is only by incorporating data from other observatories and previous epochs that we can usefully fit the SED; with this we explicitly assume no evolution of the point source between the epochs. We find that warm dust with a temperature ∼300 K distributed over a radius of 150-200 AU. We fit the far-infrared lines of CO arising from the point source, from an extended environment around V838 Mon. Assuming a model of a spherical shell for this gas, we find that the CO appears to arise from two temperature zones: a cold zone (T kin ≈ 18 K) that could be associated with the ISM or possibly with a cold layer in the outermost part of the shell, and a warm (T kin ≈ 400 K) zone that is associated with the extended environment of V838 Mon within a region of radius of ≈210 AU. The SiO lines arise from a warm/hot zone. We did not fit the lines of H 2 O as they are far more dependent on the model assumed.

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“…The eruption of V838 Mon in Feb. 2002(Munari et al 2002 reached an apparent magnitude of V = 6.7 mag and was studied quite closely. The light curve showed three maxima and a consistent change of colours redwards as the spectrum reached an L supergiant phase at the end of the year (Evans et al 2003). The resulting circumstellar light echo was used to obtain a distance estimate of 6.1 ± 0.6 kpc, corresponding to a peak absolute magnitude M V = −9.8 (Bond et al 2003;Sparks et al 2008).…”

Section: Introductionmentioning

confidence: 99%

The January 2015 outburst of a red nova in M 31

Kurtenkov

Pessev

Tomov

et al. 2015

A&A

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Context. M31N 2015M31N -01a (or M31LRN 2015 is a red nova that erupted in January 2015 -the first event of this kind observed in M 31 since 1988. Very few similar events have been confirmed as of 2015. Most of them are considered to be products of stellar mergers. Aims. Results of an extensive optical monitoring of the transient in the period January-March 2015 are presented. Methods. Eight optical telescopes were used for imaging. Spectra were obtained on the Large Altazimuth Telescope (BTA), the Gran Telecsopio Canarias (GTC) and the Rozhen 2 m telescope. Results. We present a highly accurate 70 d light curve and astrometry with a 0.05 uncertainty. The colour indices reached a minimum of 2−3 d before peak brightness and rapidly increased afterwards. The spectral type changed from F5I to F0I in 6 d before the maximum and then to K3I in the next 30 d. The luminosity of the transient was estimated to be 8.7 +3.3 −2.2 × 10 5 L during the optical maximum. Conclusions. Both the photometric and the spectroscopic results confirm that the object is a red nova, similar to V838 Monocerotis.

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V838 Mon: an L supergiant?

Cited by 67 publications

References 19 publications

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

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

On the properties of dust and gas in the environs of V838 Monocerotis

The January 2015 outburst of a red nova in M 31

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