  Context: Classical nova progenitors are cataclysmic variables and very old
novae are observed to match high mass transfer rate and (relatively) long
orbital period systems. However, the aftermath of a classical nova has never
been studied in detail. Aims: To probe the aftermath of a classical nova
explosion in cataclysmic variables and observe as the binary system relaxes to
quiescence. Methods: We used multi-wavelength time resolved optical and
near-infrared spectroscopy for a bright, well studied classical nova five years
after outburst. We were able to disentangle the contribution of the ejecta at
this late epoch using its previous characterization, separating the ejecta
emission from that of the binary system. Results: We determined the binary
orbital period (P=3.76 hr), the system separation and mass ratio (q>=0.17 for
an assumed white dwarf mass of 1.2 solar masses). We find evidence of an
irradiated secondary star and no unambiguous signature of an accretion disk,
although we identify a second emission line source tied to the white dwarf with
an impact point. The data are consistent with a bloated white dwarf envelope
and the presence of unsettled gas within the white dwarf Roche lobe.
Conclusions: At more than 5 years after eruption, it appears that this
classical nova has not yet relaxed.
