[IAUC] CBET 671: 20061012 : V2362 CYGNI

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                                                  Electronic Telegram No. 671
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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V2362 CYGNI
     U. Munari, A. Siviero, and M. Valentini, Istituto Nazionale di
Astrofisica, Padova Astronomical Observatory; and G. Cherini, S.
Dallaporta, G. Dalla Via, and S. Tomaselli, ANS (Asiago Novae and
Symbiotic stars) Collaboration, report that V2362 Cyg (N Cyg 2006; cf.
IAUC 8697, 8698, 8702) is displaying a rather peculiar behavior.  For
more than two months, it has been smoothly and slowly declining from
the maximum (B = 9.5, B-V = +0.89) reached on April 8.  In late June,
the decline abandoned the pure exponential slope and began to slow
progressively, reaching a minimum brightness of B = 12.30 around July
21, when the colors were B-V = +0.16, V-I_c = +1.28, R_c-I_c = +0.02.
Since then, the nova has been following a smooth re-brightening pattern
that has taken it to B = 11.85 and B-V = +0.21, V-I_c = +0.96, R_c-I_c
= +0.18 as mean values for the first week of October.  The optical
spectroscopic evolution has been minimal (if any at all) over the last
four months, with Balmer series, N III 464.0-nm, N II 567.9-nm, [N II]
575.5-nm, and [O I] 630.0- and 636.4-nm still dominating the
emission-line spectrum, with a stable FWHM of about 1750 km/s for
unblended lines.


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                         (C) Copyright 2006 CBAT
2006 October 12                  (CBET 671)               Daniel W. E. Green