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Nova V2362 Cygni rapidly changes spectrum

ATEL # 963; Kimeswenger, S., Dalnodar, S., Knapp, A., Schafer, J., Unterguggenberger, S., Weiss, S. (AI Innsbruck)
on 14 Dec 2006; 22:53 UT
Distributed as an Instant Email Notice (Nova)
Password Certification: Stefan Kimeswenger (

Subjects: Optical, Nova

V2362 Cygni (N Cyg 2006) had the outburst end March or early April 2006 (Nakano, IAUC 8697) and the maximum April, 6th. After a rapid decline (t3 = 19 days) it stopped its decline 4.5 mag below maximum and thereafter re brightened (Goranskij et al. ATEL #928). After V2362 Cygni (N Cyg 2006) concluded it's re brightening (2.0 mag) phase (Munari et al. CBET 769) it started a rapid decline 7 months after maximum. While the spectroscopy during the plateau changed marginally the P-Cygni absorption changed its velocity to values during main outburst (Munari et al. CBET 769). It was classified as Fe II-type CO novae (Russell et al. IAUC, 8710). While our spectrum obtained December, 7th still is dominated by the NII+[NII] blend on 570.8nm, NaI+OI blend on 592.0nm (FWHM approx 80A) and H_alpha (FWHM = 6.8nm) and tiny P-Cygni absorptions, the spectra obtained December 13th and 14th with the Innsbruck 60cm telescope, are dominated by narrow , but higher, Balmer lines (H_alpha FWHM = 3.4nm) and [NII] (567.6 nm, FWHM = 3.3nm). Weak emission of [OII] 630.0nm, 731.8nm and 732.9nm and [OI] 844.6 nm are also visible. The continuum dropped dramatically towards detection limit - line contrast H_alpha / continuum changed from 3:1 to 35:1. Although the nebular stage clearly started, excitations states of dominating lines still is very low. Continuous spectroscopic monitoring is required. The spectrum is given at

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