TY - JOUR
T1 - Nova V351 Puppis 1991
T2 - A multiwavelength study of the nebular phase
AU - Saizar, P.
AU - Pachoulakis, I.
AU - Shore, S. N.
AU - Starrfield, Sumner
AU - Williams, R. E.
AU - Rothschild, E.
AU - Sonneborn, G.
PY - 1996/1/1
Y1 - 1996/1/1
N2 - We combine ground-based optical and IUE spectrophotometry to study the physical conditions in the shell of Nova V351 Puppis 1991. The structure and the evolution of the shell during the early nebular (i.e. optically thin) phase are discussed in this paper. The reddening, derived from recombination lines, is E(B - V) = 0.72 ± 0.10. The optical/UV light curves imply a distance of 3.0 ± 0.5 kpc. These values are found to be consistent with a study of the reddening in the stellar field near the nova. Abundances from the emission-line spectra yield enhancements within the predictions of thermonuclear runaway models for classical novae. 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 (Mej ∼ 10-7 M⊙), implying a high- mass white dwarf. The optical spectra reveal a strong red excess, which we tentatively attribute to the red companion. The strength of this continuum suggests that the companion is either a giant or an irradiated main-sequence star.
AB - We combine ground-based optical and IUE spectrophotometry to study the physical conditions in the shell of Nova V351 Puppis 1991. The structure and the evolution of the shell during the early nebular (i.e. optically thin) phase are discussed in this paper. The reddening, derived from recombination lines, is E(B - V) = 0.72 ± 0.10. The optical/UV light curves imply a distance of 3.0 ± 0.5 kpc. These values are found to be consistent with a study of the reddening in the stellar field near the nova. Abundances from the emission-line spectra yield enhancements within the predictions of thermonuclear runaway models for classical novae. 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 (Mej ∼ 10-7 M⊙), implying a high- mass white dwarf. The optical spectra reveal a strong red excess, which we tentatively attribute to the red companion. The strength of this continuum suggests that the companion is either a giant or an irradiated main-sequence star.
KW - Novae, cataclysmic variables
KW - Stars: individual: Nova Puppis 1991
KW - Ultraviolet: stars
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U2 - 10.1093/mnras/279.1.280
DO - 10.1093/mnras/279.1.280
M3 - Article
AN - SCOPUS:0008670384
VL - 279
SP - 280
EP - 292
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 1
ER -