Basic system parameters and a more general SPOT solution of the SV Camelopardalis light curve

Details Basic system parameters and a more general SPOT solution of the SV Camelopardalis light curve Basic system parameters and a more general SPOT solution of the SV Camelopardalis light curve

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292..119p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 1, p. 119-124

Statistics

Computation

19

Computational Astrophysics, Eclipsing Binary Stars, Light Curve, Mass Ratios, Parameter Identification, Stellar Mass, Stellar Rotation, Sun, Astronomical Models, Astronomical Observatories, Correlation, Doppler Effect, Imaging Techniques, Nonlinearity, Stellar Models

Scientific paper

SV Cam has been monitored at Konkoly Observatory since 1973. Based on these data we have chosen the light-curve best suitable for the determination of the system parameters and we rediscuss the eclipse parameters of the binary system suggesting a mass ratio of m2/m1 = 0.6. Although the effect of spottedness on this particular light-curve was relatively low we analyze it in a second step to derive spot parameters. Under the assumption of maximum contrast between a stellar spot and its surroundings, Zeilik et al. (1988) analyzed the SV Cam light curve and derived spot parameters of the primary star in the binary system. We base our analysis on another model of an extended active region and spot group, because this is the usually observed inhomogeneous structure on the Sun. In our model the spot filling factor inside the active region is a free parameter, and hence the mean contrast of the spot group, too. We find a strongly nonlinear correlation between the contrast and the stellar latitude solutions.

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