| Autor: |
Munari, U., Corradi, R. L. M., Henden, A., Navasardyan, H., Valentini, M., Greimel, R., Leisy, P., Augusteijn, T., Djupvik, A. A., Glowienka, L., Somero, A., de la Rosa, I. G., Vazdekis, A., Kolka, I., Liimets, T., Munari, U., Corradi, R. L. M., Henden, A., Navasardyan, H., Valentini, M., Greimel, R., Leisy, P., Augusteijn, T., Djupvik, A. A., Glowienka, L., Somero, A., de la Rosa, I. G., Vazdekis, A., Kolka, I., Liimets, T. |
| Zdroj: |
Astronomy and Astrophysics; November 2007, Vol. 474 Issue: 2 p585-590, 6p |
| Abstrakt: |
After four years during which only the spectacular light echo was showing continuous and rapid evolution while the central star was nearly constant, in autumn 2006 V838 Mon began a sequence of events which profoundly altered its spectroscopic and photometric behavior: (a) an eclipse of the B3V companion, characterized by the disappearance and reappearance of the B3V companion from optical spectra, and an eclipse-like lightcurve of ~70 day duration and $\Delta B \sim 1.15$mag, $\Delta V \sim 0.55$mag, $\Delta R_{\rm C} \sim 0.10$mag maximum depth; (b) a large increase in intensity of the [FeII] and FeII emission lines, and the appearance in emission for the first time since the 2002 outburst of Hαand higher Balmer series lines. While the [FeII] and FeII lines maintained a very sharp and unresolved profile, the Hαdeveloped into a wide and structured profile, characterized by a sharp central reversal at the same velocity as one of the CO radio emission components. The disappearance of the B3V companion is equally well explained by a grazing eclipse from the outbursting L-type supergiant or by an eclipse from a dust cloud characterized by $E_{B-V}=0.55$and $R_{V}=3.1$. We believe the flaring of the emission lines occurred at a similar time as the B3V eclipse just by chance. |
| Databáze: |
Supplemental Index |
| Externí odkaz: |
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