Abstract
We present BVRC differential photometry of an eclipsing binary system V826 Aur. A period analysis shows near constant period of 0.36 days across two decades of observation. The best fit models are consistent with a W-type W UMa overcontact binary consisting of a less massive G8 primary star and a more massive K0 secondary star. The modeled system properties are unremarkable with mass ratio (q=2.9), inclination (i=82°), fillout factor (f=0.094), and temperature ratio (T2/T1=0.96), all near the average for W-type systems. A very slight O’Connell effect is present and is analyzed. A cool spot is used to model the effect, resulting in fitted spot parameters of angular size (ρ=8.2°), temperature factor (κ=0.81), and longitude (λ=63°) while colatitude was fixed at 90°.
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