Nova V2362 Cygni increases its brightness
ATel #928; Goranskij, V. P., Metlova, N. V. (SAI, Moscow Univ.), and Burenkov, A. N. (Special Astrophysical Observatory, Russia)
on 1 Nov 2006; 19:44 UT
Credential Certification: Vitaly Goranskij (goray@sai.msu.ru)
Subjects: Optical, Binary, Nova
Classical nova V2362 Cyg (N Cyg 2006, 23:11:32.34, +44:48:03.9, 2000) undergoes gradual increase of its brightness since middle of August, 2006 from the level of V = 11.9. In October 27, 2006 it has reached V = 11.26. The rate of this brightening is rising during the last week. This development resembles the scenario of V1493 Aql with the large hump superimposed on the descending branch of the light curve.
We performed CCD V monitoring of this nova in 11 nights between 2006 August 19 and 31 using 50-cm Maksutov telescope of SAI Crimean Station. Nova shows variations in the time scale of hours with the amplitude of 0.11 mag. Fourier analysis reveals the pronounced periodicity of 0.2070 day with the aliases at 0.1714 and 0.2612 days.
We analysed the spectra of V2362 Cyg taken with 1-m telescope of SAO on 2006 October 27 and 28 (spectral range 3800-7530A, resolution FWHM = 4.6 and 8.7A). The Balmer lines and a few other emission features have very wide multiple-peak asymmetric profiles. The full width of Halpha line is 5900 km/s, and that one of Hbeta is 5300 km/s. We identified the strongest emission features as CIII+NIII blend centered on 4652A, [OIII]+NII blend on 5010A, NII+[NII] blend on 5708A, NaI+OI blend on 5920A. Absence of HeI lines at 6678 and 7065A is surprising. So, nova is not yet entered the nebular stage. This may be a high inclined binary at the end of common envelope phase. Its monitoring is of interest.
The details of photometry and spectroscopy
