Modeling the Eclipses of the Classical Nova QU Vulpeculae and the Novalike Variable LX Serpentis

Details Modeling the Eclipses of the Classical Nova QU Vulpeculae and the Novalike Variable LX Serpentis Modeling the Eclipses of the Classical Nova QU Vulpeculae and the Novalike Variable LX Serpentis

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5108m&link_type=abstract

American Astronomical Society, AAS Meeting #211, #51.08; Bulletin of the American Astronomical Society, Vol. 39, p.816

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Scientific paper

Multicolor (BVRI) eclipse light curves of the nova-like variable LX Ser and the classical nova QU Vul have been analyzed with a parameter-fitting eclipse model. The R-band eclipses of QU Vul were found to be surprisingly shallow relative to eclipses in the other colors. In order to achieve a plausible fit to the data it was necessary to assume that 20 percent of the out-of-eclipse light in R results from contamination by an uneclipsed source of H-alpha light in this system. Although the mass ratios (q=M2/M1) of both systems are poorly constrained, the best-fitting models are characterized by mass ratios of q = 0.5 (i = 79.0 deg), and q = 0.2 (i = 80.75 deg) for LX Ser and QU Vul, respectively. The accretion disk parameters of LX Ser were relatively well constrained, with our models suggesting a disk that extends to approximately 65 percent of the distance to the inner Lagrangian point (near the maximum allowed for a tidally truncated disk), and having a radial temperature profile flatter than that expected for a steady-state disk. The accretion disk parameters of QU Vul, however, were more poorly constrained. The more extreme mass ratio for this system results in a significant portion of the outer disk remaining uneclipsed at superior conjunction of the white dwarf. We show that the eclipse depths for QU Vul can be equally well fit by a cool, low-luminosity disk with a relatively flat temperature profile, or by a hotter, more luminous disk with steeper temperature profile.

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