  We present BVR observations of DK CVn from 2007 and 2008. We analysed the BVR
light curves of the system and obtained the system's parameters. Using the
`q-search' method, we measured the mass ratio of the system (q) as 0.55. Taking
the temperature of the primary component as 4040K, the temperature of the
secondary was found to be 3123K. Several flares were detected, and the
distributions of flare equivalent duration versus flare total duration were
modelled using the One-Phase Exponential Association Function for these flares.
The parameters of the model demonstrated that the flares are the same as those
detected from UV Ceti stars. We also demonstrate that the variation at
out-of-eclipse must be caused by some cool spot(s) on one of the components.
The star is found to show two active longitudes in which the spots are mainly
formed. Consequently, this study reveals that DK CVn should be a
chromospherically active binary star.
