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Nova V351 Puppis 1991: a multiwavelength study of the nebular phase
We combine ground-based optical and IUE spectrophotometry to study thephysical conditions in the shell of Nova V351 Puppis 1991. The structureand the evolution of the shell during the early nebular (i.e. opticallythin) phase are discussed in this paper. The reddening, derived fromrecombination lines, is E(B-V)=0.72+/-0.10. The optical/UV light curvesimply a distance of 3.0+/-0.5 kpc. These values are found to beconsistent with a study of the reddening in the stellar field near thenova. Abundances from the emission-line spectra yield enhancementswithin the predictions of thermonuclear runaway models for classicalnovae. Relative to solar by number, they are: He/H=1.7, C/H=3.5,N/H=130, O/H=38, Ne/H=120, Al/Si=28. The shell shows a low ejected mass(M_ej~10^-7 M_solar), implying a high-mass white dwarf. The opticalspectra reveal a strong red excess, which we tentatively attribute tothe red companion. The strength of this continuum suggests that thecompanion is either a giant or an irradiated main-sequence star.
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Observation and Astrometry data
| Constellation: | Πρύμνη |
| Right ascension: | 08h18m57.31s |
| Declination: | -39°04'44.6" |
| Apparent magnitude: | 7.072 |
| Distance: | 653.595 parsecs |
| Proper motion RA: | 2.8 |
| Proper motion Dec: | -1 |
| B-T magnitude: | 7.005 |
| V-T magnitude: | 7.067 |
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