Spectroscopic observations of PU Vulpeculae in the 3210-10950 A range during the nebular phase.

Spectroscopic observations of PU Vulpeculae have been carried out at the Observatoire de Haute-Provence from 1989 June to 1992 September during a decline of brightness from 10.1 to 11.2 in visual magnitude. A spectral type M6III may be proposed for the cool component from TiO band intensities, while the hot surrounding gas is responsible for about 280 emission lines (many of which belong to Fe+ and Fe+ + ions), many of which undergo variations in intensity. Analysis of the [0 iiij lines reveals a kinetic temperature of about 12000 K and a lower limit for the electron density of 6.7 x 10 in 1991 October, decreasing by a factor of 2-3 by 1992 September. Helium may be slightly overabundant (by a factor of 2) with respect to the solar value. Key words: line: identification - stars: individual: PU Vni - novae, cataclysmic variables.