Nova V2362 Cygni increases its brightness

Goranskij, V.P., Metlova, N.V. (SAI, Moscow University); Burenkov, A.N. (Special Astrophysical Observatory, Russia)

To be published in Astronomer's Telegram No. 928.

Classical nova V2362 Cyg (N Cyg 2006, 21:11:32.34, +44:48:03.9, 2000 [position in ATel 928 is incorrect!]) 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 pronounced periodicity of 0.2070 day with aliases at 0.1714 and 0.2612 days.

Fig. 1. Amplitude spectrum of V2363 Cyg.

Fig. 2. The light curve of V2363 Cyg folded with the period of 0.2070 day.

We analysed 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. 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.

Fig. 3. The spectrum of V2363 Cyg taken on 2006 Oct 26, and line identifications.

View UBVRc light curves of V2362 Cyg. Java compatible brouser is needed. Use mouse mouseDrag function to examine the details.