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G. J. Schwarz (Steward Observatory)
This paper presents a new analysis of the moderately fast ONeMg nova QU Vul 1984 using published ultraviolet, optical, infrared and radio observations. The technique uses an optimization code in combination with Cloudy photoionization models to fit the emission line spectra obtained at four epochs during the nebular phase of the outburst. Previous studies of QU Vul yielded considerable differences in the derived elemental abundances, ejected mass and distance. This analysis, which is consistent with all the available data and over multiple epochs, generally finds the lowest abundance enhancements of the previous studies. The distance most compatible with the all of the available distance determinations is 2.4 kpc. Given this distance, the ejected mass is very high with a value of ~ 5e-4 solar masses. Relative to other ONeMg novae, the lower elemental enhancement and large ejected mass estimate, coupled with the long lightcurve decay time and nuclear burning timescale implies that the outburst occurred on a low mass ONeMg white dwarf. An important test of this hypothesis would be a determination of the WD mass in this system.
The author(s) of this abstract have provided an email address for comments about the abstract: gschwarz@as.arizona.edu
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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.