Volume 460, Number 1, December II 2006
|Page(s)||245 - 250|
|Section||Stellar structure and evolution|
|Published online||12 September 2006|
The properties of V838 Monocerotis in 2002 November
Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Hertfordshire AL10 9AB, UK e-mail: firstname.lastname@example.org
2 Main Astronomical Observatory, Academy of Sciences of the Ukraine, Golosiiv Woods, Kyiv-127, 03680, Ukraine
3 Astrophysics Group, School of Physical & Geographical Sciences, Keele University, Keele Staffordshire, ST5 5BG, UK
4 Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720-3411, USA
Accepted: 4 September 2006
We present the results of modelling the 0.45–1m spectral energy distribution of V838 Mon for 2002 November. Synthetic spectra were calculated using the NextGen model atmospheres of Hauschildt et al. (1999, ApJ, 512, 377), which incorporate line lists for H2O, TiO, CrH, FeH, CO, and MgH, as well as the VALD atomic line list. Fits to the observed spectra show that, in 2002 November, the effective temperature of V838 Mon was approximately K. Our theoretical spectra show a comparatively weak dependence on . Preliminary analysis of the hot star observed together with V838 Mon shows it to be a normal B3V dwarf.
Key words: stars: individual: V838 Mon / stars: atmospheres / stars: evolution
© ESO, 2006
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