The peculiar variable V838 Mon

  title={The peculiar variable V838 Mon},
  author={Stefan Kimeswenger and Cheryl Lederle and Stefan Schmeja and B. Armsdorfer},
  journal={Monthly Notices of the Royal Astronomical Society},
V838 Mon underwent, after a first nova-like outburst in January and a usual decline, a second outburst after one month, and a third weak one again a month later. Moreover, a very small increase of the temperature at the beginning of April gives us a hint about a physical process with a period of one month. We obtained a BV R IC time-sequence and modelled the photometric behaviour of the object. This leads us to the conclusion that the interstellar foreground extinction has to be 0.6 mag E(B − V… 
The post-outburst photometric behaviour of V838 Mon
The unusual eruptive variable discovered in Monoceros in 2002 January underwent dramatic photometric and spectroscopic changes in the months prior to its 2002 June‐August conjunction with the Sun.
Evolution of V838 Monocerotis during and after the 2002 eruption
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 peculiar variable V838 Monocerotis
Spectroscopic observations of the peculiar variable V838 Mon during the period from the second light outburst until the fast dimming are presented. We describe high resolution (R ≈ 60 000) high S /N
On the progenitor of V838 Monocerotis
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
An analysis of a spectrum of V838 Monocerotis in October 2005
Context. V838 Mon erupted at the beginning of 2002 becoming an extremely luminous star with $L=10^6~L_{\sun}$. Among various scenarios proposed to explain the nature of the outburst, the most
Progenitor and Remnant of the Luminous Red Nova V838 Monocerotis
Abstract —The article presents the results of multicolor photometry, medium and low resolution spectroscopy of the red nova V838 Mon remnant for 16 years after the 2002 outburst. We also used the
V4332 Sgr in `Quiescence'
In 1994 V4332 Sgr underwent a mysterious eruption. Somehow its fast evolution towards a red giant star was, lacking alternative classifications, connected to the red variable M31 RV, which had its
V838 Monocerotis (V838 Mon) erupted at the beginning of 2002 becoming an extremely luminous star with L ≃ 106L☉. Among various scenarios proposed to explain the nature of the outburst, the most
A model of an expanding giant that swallowed planets for the eruption of V838 Monocerotis
ABSTRACT In early 2002 V838 Monocerotis had an extraordinary outburst whose nature isstill unclear. The optical light curve showed at least three peaks and imaging revealeda light echo around the
The planets capture model of V838 Monocerotis: conclusions for the penetration depth of the planet(s)
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


The mysterious eruption of V838 Mon
V838 Mon is marking one of the most mysterious stellar outbursts on record. The spectral energy distribution of the progenitor resembles an under-luminous F main sequence star (at V =1 5:6 mag), that
Nova Sagittarii 1994 1 (V4332 Sagittarii): The Discovery and Evolution of an Unusual Luminous Red Variable Star
We report photometry and spectroscopy of the evolution of Nova Sagittarii 1994 1 (V4332 Sagittarii) during outburst. We compare the photometric and spectral evolution of this outburst with known
Revised Analysis of the Supersoft X-Ray Phase, Helium Enrichment, and Turnoff Time in the 2000 Outburst of the Recurrent Nova CI Aquilae
Recurrent nova CI Aquilae entered the final decline phase a bit before 2001 May, about 300 days after the optical maximum, showing the slowest evolution among recurrent novae. Based on the optically
Rare thermonuclear explosions in short-period cataclysmic variables, with possible application to the nova-like red variable in the Galaxy M31
A very bright nova with a peak luminosity significantly larger than the relevant Eddington luminosity might be initiated by a hydrogen shell flash on a very cold low-mass degenerate dwarf accreting
Prediction of supersoft x-ray phase, helium enrichment, and turn-off time in recurrent nova ci aquilae 2000 outburst
Recurrent nova CI Aquilae is still bright 300 days after the optical maximum, showing the slowest evolution among recurrent novae. We predict the turn-off time of CI Aql 2000 outburst coming in
The Anomalous Infrared Emission of Abell 58
We present a new model to explain the excess in mid- and near-infrared emission of the central, hydrogen-poor dust knot in the planetary nebula (PN) Abell 58. Current models disagree with ISO
The nature of recurrent novae
The observational properties and outburst histories of each member of the small class of recurrent novae are reviewed, with the objective of identifying the outburst mechanisms for these systems.
For 31 classical galactic novae and four recurrent novae distances, absolute magnitudes and extinction data are derived by different methods. A new absolute magnitude - t3 time relation is
The dusty universe