THE TEMPORAL EVOLUTION OF THE 4-14 MICRON SPECTRUM OF V1974 CYGNI (NOVA CYGNI 1992)

We present 4-14 mu m spectra of the ONeMg nova V1974 Cygni (Nova Cygni 1992) obtained during 1992 May on the NASA Kuiper Airborne Observator y (KAO) and from the NASA 1.52 m infrared telescope at Mount Lemmon, A rizona in 1992 October/November with the HIFOGS mid-infrared spectrome ter. The spectra at both epochs showed continuum emission from thermal bremstrahlung (free-free radiation) with emission lines from hydrogen and [Ne II], [Ar III], and [Ne VI]. During May, approximate to 80 day s after outburst, the dominant emission lines in the mid-infrared spec tra were a blend of three hydrogen lines (Pf alpha, Hu beta, H11-7) ne ar 7.5 mu m and [Ne II] at 12.8 mu m. By October (approximate to 160 d ays later), the hydrogen emission had virtually disappeared, the [Ne I I] 12.8 mu m line had weakened considerably, and a pronounced [Ne VI] emission line had appeared at 7.6 mu m. This behavior confirms that V1 974 Cyg is similar to the prototypical slow ONeMg ''neon nova,'' Nova QU Vulpeculae (1984 No. 2). The remarkable evolution of the spectrum s uggests that the ionization conditions changed drastically between 199 2 May and 1992 October. We find that the ejecta of V1974 Cyg were over abundant in neon with respect to silicon by a factor of approximate to 10 relative to the solar photosphere. We present new model calculatio ns of infrared sodium forbidden line emission from [Na III] 7.319 mu m , [Na IV] 9.039 mu m, and [Na IV] 21.29 mu m that can be compared with recent model predictions of sodium synthesis in ONeMg nova outbursts. We conclude that sodium abundances in ONeMg novae can be determined b y observations of infrared coronal lines of sodium that are accessible to the Infrared Space Observatory (ISO) and instruments at the NASA I RTF.