Other
Scientific paper
Feb 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...440..336c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 440, no. 1, p. 336-344
Other
5
Astronomical Photometry, Cataclysmic Variables, Eclipsing Binary Stars, Novae, Stellar Color, Stellar Models, Stellar Temperature, Accretion Disks, Light Curve, Mathematical Models, Power Series, Temperature Profiles, Temporal Resolution, White Dwarf Stars
Scientific paper
Time-resolved photometric observations of the V = 17 mag classical nova QZ Aur (Nova Aur 1964) are presented. These data reveal QZ Aur to be eclipsing with an orbital period of 0.357496 days (8.58 hr). A total of 10 eclipses were obtained during a 3 yr period spanning 1990-1992. These data include at least two eclipses in each of four broadband colors (B, V, R, and I). The eclipse depth (approximately 1.2 mag in B) indicates that the white dwarf and central disk region must be occulted at mid-eclipse. The eclipse profiles were simulated using a simple parameter-fitting model similar to that employed by Zhang in his studies of HT Cas, U Gem, and AC Cnc. Although the mass ratio of QZ Aur is unknown, many of the parameters in our model are well constrained by the data. The full width of the eclipse indicates that the accretion disk is significantly larger than its zero-viscosity radius and extends to approximately 65% of the distance from the white dwarf to the inner Lagrangian point. The temperature profile of the accretion disk is modeled as a power law: T(R) proportional to R-alpha. The optimum value of alpha is approximately 0.55 -- somewhat smaller than the value of 0.75 expected for an optically thick, steady state disk, but not atypical of other novae and nova-like variables. We find that the secondary star in QZ Aur has a temperature of 5200 K, suggesting a spectral type near K0 V. The expected flux from the secondary star is used to estimate a distance of 2.0 +/- 0.4 kpc to the QZ Aur system.
Campbell Randall D.
Shafter Allen W.
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