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Context: Optical nova lightcurves often have structures, such as rapiddeclines and recoveries, due to nebular or dusty phases of the ejecta. NovaCygni 2006 (V2362 Cyg) underwent an unusual brightening after an early rapiddecline. The shape of the lightcurve can be compared to that of V1493 Aql, butthe whole event in that case was not as bright and only lasted a couple ofweeks. V2362 Cyg had a moderately fast decline of t_2 = 9.0 beforerebrightening, which lasted 250 days after maximum. Aims: We present ananalysis of our own spectroscopic investigations in combination with AAVSOphotometric data covering the whole rebrightening phase until the return to thefinal decline. Methods: We used the medium resolution spectroscopy obtained inten nights over a period of 79 nights to investigate the change of the velocitystructure of the ejecta. The publicly available AAVSO photometry was used toanalyze the overall properties and the energy of the brightening. Results:Although the behavior of the main outburst (velocity, outburst magnitude, anddecline timescales) resembles a ``normal'' classical nova, the shell clearlyunderwent a second fast mass ejecting phase, causing the unusual properties.The integrated flux during this event contributes ~ 40 % to the total radiationenergy of the outburst. The evolution of the H_alpha profile during the bumpevent is obtained by subtracting the emission of the detached shells of themain eruption by a simple optically thin model. A distance of D ~ 7.5{+3.0}{-2.5} kpc and an interstellar extinction E(B-V) = 0.6 +/- 0.1 was alsoderived.

The unusual Nova Cygni 2006 (V2362 Cyg)