The Coronal Line Region of Nova QU VUL 1984

Details The Coronal Line Region of Nova QU VUL 1984 The Coronal Line Region of Nova QU VUL 1984

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.2811s&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #28.11; Bulletin of the American Astronomical Society, Vol. 24, p.772

Astronomy and Astrophysics

Astronomy

Scientific paper

We have combined optical and ultraviolet spectrophotometry to study the physical conditions in the ejected shell of Classical Nova QU Vul 1984. In a previous paper (Saizar et al., 1992, subm. to ApJ), we have shown that a hot gas phase is present which dominates both the mass and the energetics of the ejecta. A more detailed study of this region is presented. A featureless continuum spectrum, with little or no Balmer jump present, is the clearest signature of the hot gas. From the strengths of the ultraviolet continuum and the Balmer Jump, we set a lower limit to the temperature of the coronal line region of Tcor > 8*E(4) K ~ 8times Tneb, the temperature of the ``nebular'' region where the lower ionization lines arise. The gas velocity deduced from the FWHM of several lines suggests that the hotter gas might be moving faster. We use radiative--equilibrium photoionization model calculations to predict the emission--line fluxes and the continuous spectrum at day 554. We compare several model results to the observations in order to set additional constraints on the geometry, temperature and density of the hot gas. PS acknowledges support by NASA grant NAG 5-481.

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