Context : Optical nova lightcurves often have structures , such as rapid declines and recoveries , due to nebular or dusty phases of the ejecta .
Nova Cygni 2006 ( V2362 Cyg ) underwent an unusual brightening after an early rapid decline .
The shape of the lightcurve can be compared to that of V1493 Aql , but the whole event in that case was not as bright and only lasted a couple of weeks .
V2362 Cyg had a moderately fast decline of t _ { 2 } = 9.0 \pm 0.5 days before rebrightening , which lasted 250 days after maximum .

Aims : We present an analysis of our own spectroscopic investigations in combination with American Association of Variable Star Observers ( AAVSO ) photometric data covering the whole rebrightening phase until the return to the final decline .

Methods : We used the medium resolution spectroscopy obtained in ten nights over a period of 79 nights to investigate the change of the velocity structure of the ejecta .
The publicly available AAVSO photometry was used to analyze the overall properties and the energy of the brightening .

Results : Although the behavior of the main outburst ( velocity , outburst magnitude , and decline timescales ) resembles a “ normal ” classical nova , the shell clearly underwent a second fast mass ejecting phase , causing the unusual properties .
The integrated flux during this event contributes \approx 40 % to the total radiation energy of the outburst .
The evolution of the H _ { \alpha } profile during the bump event is obtained by subtracting the emission of the detached shells of the main eruption by a simple optically thin model .
A distance of D \approx 7.5 ^ { +3.0 } _ { -2.5 } kpc and an interstellar extinction E ( B - V ) = 0 \aas@@fstack { m } 6 \pm 0 \aas@@fstack { m } 1 was also derived .

Conclusions :