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Session 27 - Variable Stars, Novae, & Supernovae.
Display session, Tuesday, June 10
South Main Hall,
Photometric data (Howell 1989) for the cataclysmic variable AR Cnc were analyzed using the Wilson-Devinney differential corrections program. The three light curves (two in B and one in V) were studied to find a consistent set of geometrical and astrophysical parameters which provided the best weighted least-squares fit to the data. Free parameters included inclination (i), the temperature of the secondary (T2), potential of the primary (omega 1), mass ratio (q), luminosity of the primary (L1), and third light (l3). Lack of definitive spectroscopy for the primary component further complicated the solution as it was necessary to assume a primary temperature of 20,000K based on limitations cited for similar systems such as DV UMa. Nonetheless, calculated temperatures for the secondary (which are correlated to the assumed temperature of the primary) lay in the expected range for the cited M$ spectral classification of the secondary component. Physical conditions of the system such as the faintness of the system, and hence the rms variations in the observations, and the narrowness and depth of primary eclipse strongly controlled the selection of parameter subsets in the differential corrections sequence. This is also discussed with the light curve analysis.
References: Howell, S. et al, 1989 PASP, 102, 758-772
