HOT GAS AND THE ORIGIN OF THE NEBULAR CONTINUUM IN NOVAE

A featureless blue continuum (with constant f(v)) is a defining featur e of declining classical novae. The fact that f(v) is constant into th e infrared, and the absence of a Balmer jump, suggests that this conti nuum originates in hot tenuous gas. The electron temperature and densi ty of the hot gas phase of classical nova QU Vul 1984 are estimated fr om ground-based optical and IUE ultraviolet observations. This region has a temperature of 10(5)-10(6) K, and a density in the range of 2 x 10(4) to 3 x 10(5) cm(-3). In addition, a colder, denser shell compose d of many ''clumps'' or condensations is present, and it is responsibl e for most of the optical-to-ultraviolet emission lines. The hot gas, however, may be much more massive and could dominate the energetics of the ejecta. The total returned mass could be as high as 10(-4) and 4 x 10(-3) M. depending on conditions in the hot gas. The large mass of the shell, in combination with the high metallicity found in this nova , supports the idea that novae may be an important contributor to the chemical enrichment of the interstellar medium.