TY - JOUR
T1 - The temporal evolution of the 1-5 micron spectrum of V1974 Cygni (Nova Cygni 1992)
AU - Woodward, Charles E.
AU - Greenhouse, Matthew A.
AU - Gehrz, R. D.
AU - Pendleton, Y. J.
AU - Joyce, R. R.
AU - Van Buren, D.
AU - Fischer, J.
AU - Jennerjohn, N. J.
AU - Kaminski, C. D.
PY - 1995/1/10
Y1 - 1995/1/10
N2 - We present 1-5 μm moderate- and high-resolution infrared spectra of the ONeMg nova V1974 (Nova Cygni 1992) obtained at multiple epochs during an ≈500 day period after outburst. During the first 80 days, the spectra exhibited continuum emission from thermal bremsstrahlung (free-free radiation) with prominent recombination line emission from hydrogen, helium, nitrogen, and oxygen. The measured FWHM of these recombination lines suggests that the initial velocity of the ejecta was ≈2400-3400 km s-1. We estimate from the hydrogen recombination line ratios that the density of the ionized shell at this epoch was ≈109 cm-3, with an effective electron temperature of ≈5 × 103 K. As the temporal evolution of the ejecta progressed, the hydrogen and helium lines diminished in intensity, and coronal lines of aluminum, calcium, magnesium, neon, and sulfur appeared by ≈day 80. The coronal line emission phase persisted for over 400 days. During this epoch, no significant dust formation occurred. We find that the ejecta of V1974 Cyg were overabundant in aluminum with respect to silicon by a factor of ≈5 and in magnesium with respect to silicon by a factor of > 3 relative to the solar photosphere. Comparison of our observed overabundances with recent model predictions of elemental synthesis in ONeMg outbursts suggests that the accreted envelope on V1974 Cyg was close to solar composition and that the precursor ONeMg white dwarf had a mass of ≈1 M⊙.
AB - We present 1-5 μm moderate- and high-resolution infrared spectra of the ONeMg nova V1974 (Nova Cygni 1992) obtained at multiple epochs during an ≈500 day period after outburst. During the first 80 days, the spectra exhibited continuum emission from thermal bremsstrahlung (free-free radiation) with prominent recombination line emission from hydrogen, helium, nitrogen, and oxygen. The measured FWHM of these recombination lines suggests that the initial velocity of the ejecta was ≈2400-3400 km s-1. We estimate from the hydrogen recombination line ratios that the density of the ionized shell at this epoch was ≈109 cm-3, with an effective electron temperature of ≈5 × 103 K. As the temporal evolution of the ejecta progressed, the hydrogen and helium lines diminished in intensity, and coronal lines of aluminum, calcium, magnesium, neon, and sulfur appeared by ≈day 80. The coronal line emission phase persisted for over 400 days. During this epoch, no significant dust formation occurred. We find that the ejecta of V1974 Cyg were overabundant in aluminum with respect to silicon by a factor of ≈5 and in magnesium with respect to silicon by a factor of > 3 relative to the solar photosphere. Comparison of our observed overabundances with recent model predictions of elemental synthesis in ONeMg outbursts suggests that the accreted envelope on V1974 Cyg was close to solar composition and that the precursor ONeMg white dwarf had a mass of ≈1 M⊙.
KW - Infrared: stars
KW - Novae, cataclysmic variables
KW - Stars: abundances
KW - Stars: individual (Nova Cygni 1992)
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U2 - 10.1086/175134
DO - 10.1086/175134
M3 - Article
AN - SCOPUS:11944267805
SN - 0004-637X
VL - 438
SP - 921
EP - 931
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -