Abstract
Astrophysical parameters of classical nova outbursts that can be quantified by infrared (IR) measurements are reviewed. Recent observational results on V1974 Cyg (a neon nova) and Nova Cas 1993 (an extreme DQ Her-type CO nova) are reported. The data imply that the ejecta of these novae were extremely overabundant in C, Ne, Mg, Al, and Si. We suggest that the abundance anomalies inferred for V1974 Qyg from IR forbidden emission line measurements apparently require that the thermonuclear runaway (TNR) excavate substantial quantities of material from the white dwarf in ONeMg nova systems. Analysis of the visual and infrared light curves of Nova Cas 1993 suggests that the grains in the dust shell grew to radii of ≈ 0.55 µm. We argue that when CO novae form visually optically thick dust shells, the dust shells probably effectively cover the central engine in almost all cases.
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Gehrz, R.D. (1995). Infrared Observations of Classical Novae: Physical Parameterization and Contributions to the ISM. In: Bianchini, A., Valle, M.D., Orio, M. (eds) Cataclysmic Variables. Astrophysics and Space Science Library, vol 205. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0335-0_4
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