INFRARED OBSERVATIONS OF DUST FORMATION AND CORONAL EMISSION IN NOVA-AQUILAE 1995

We report 1.25-18.5 mu m infrared spectrophotometric measurements of N ova Aquilae 1995. Photometric measurements were obtained over a four m onth period following the formation of an optically thin dust shell. H ydrogen and helium emission lines were evident throughout this period, along with strong near-infrared coronal line emission that appeared a pproximately 120 days after outburst. Both the photometric and the spe ctroscopic data suggest that the ejecta were clumpy, and that they con tained both a dust component and a hot gas component. The outflow velo city of the ionized ejecta was observed to be similar to 1365-1600 km s(-1) (FWHM), and no appreciable deceleration of the ejecta was observ ed over the duration of these observations. Based on a M(v)-t(2) light decline relationship, we calculate a distance of similar to 3.6-4.8 k pc.