2006CBET..739....1M

U. Munari, A. Siviero, and H. Navasardyan, Istituto Nazionale di Astrofisica, Padova Astronomical Observatory; and P. Valisa, G. Dalla Via, G. Cardarelli, G. Cherini, S. Dallaporta, S. Moretti, S. Tomaselli, P. Ochner, A. Frigo, and S. Tomasoni, ANS ("Asiago Novae and Symbiotic stars") Collaboration, write that intensive monitoring carried out with the Asiago 1.82-m telescope and other telescopes operated by the ANS Collaboration shows that V2362 Cyg (N Cyg 2006) is further developing along the peculiar behavior described in CBET 671. Following the minimum brightness of B = 12.25 reached around July 21 (when the colors were B-V = +0.16, V-I_c= +1.25, and R_c–Ic = +0.02), the nova continues its smooth re-brightening that has brought it to B = 11.18, B-V = +0.36, V-I_c = +1.10, and R_c–Ic = +0.42 by Nov. 12.8 UT – i.e., at the same brightness level that the nova had around April 23, two weeks past maximum. The mean re-brightening rates over the last 20 days have been -0.025, -0.030, -0.028, and -0.038 mag/day for B, V, R_c, and I_c, respectively. A major change occurred in the optical spectra over the last two weeks, with the reappearance on the Balmer-emission-line profiles of the two strong and blue-shifted absorption components that were visible for only a few days around maximum brightness, which had disappeared soon after; on Apr. 8.12, they were located at heliocentric velocities -1805 and -825 km/s, but in Nov. 5.76 spectra, they reappeared at -2215 and -931 km/s with equivalent widths of 0.84 and 0.22 nm and FWHM of 0.86 and 0.35 nm, respectively. These absorption components had not been present in spectra secured on Oct. 27. The most recent spectra obtained on Nov. 13.88 show the emission line profiles to be still very similar to those of Nov. 5.76.