Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003arep...47..777k&link_type=abstract
Astronomy Reports, vol. 47, Issue 9, p.777-788
Astronomy and Astrophysics
Astronomy
7
Scientific paper
New results of UBV JHKLM photometry of the symbiotic Mira V407 Cyg performed in 1998 2002 are reported. In 2002, these observations were supplemented with RI observations and a search for rapid variability in the V band. The hot component of V407 Cyg experienced a strong flare in 1998, which was the second in the history of photometric observations of this star; this flare is still continuing. During the flare, the spectral energy distribution of the hot component can be approximated by blackbody radiation with a temperature of ˜7200 K. At the maximum brightness, the bolometric flux from the hot component did not exceed 3% of the Mira's mean bolometric flux, while its bolometric luminosity was ˜400L&sun;. Appreciable variations of the star's BV brightness on a timescale of several days have been observed. These variations are not correlated with variations of B-V. Flickering on a timescale of several minutes with an amplitude of has been detected in the V band. The observations suggest that the hot component can be in three qualitatively different states. In a model with a rapidly rotating white dwarf, these states can be associated with (i) the quiescent state of the white dwarf (with a very low accretion rate), (ii) an ejection state, and (iii) an accretion state. The Mira pulsation period P is &
$ ≈ 762mathop dlimits_. 9$
; , with its infrared maximum occurring ˜0.15P after the visual maximum. A “step” is observed on the ascending branch of the Mira infrared light curves. In 1998, the gradual increase of the mean K brightness of the Mira that had been observed since 1984 was interrupted by an unusually deep minimum, after which the mean level of the K brightness considerably decreased.
Kolotilov Eugenii A.
Shenavrin V. I.
Shugarov Sergei Yu.
Yudin Boris F.
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