  We present the findings about chromospheric activity nature of KOI-256
obtained from the Kepler Mission data. Firstly, it was found that there are
some sinusoidal variations out-of-eclipses due to cool spot activity. The
sinusoidal variations modelled by the SPOTMODEL program indicate that the
active component has two different active regions. Their longitudinal variation
revealed that one of them has a migration period of 3.95 years, while the other
has a migration period of 8.37 years. Secondly, 225 flares were detected from
the short cadence data in total. The parameters, such as increase (Tr) and
decay (Td) times, total flare time (Tt), equivalent durations (P), were
calculated for each flare. The distribution of equivalent durations versus
total flare times in logarithmic scale is modelled to find flare activity
level. The Plateau value known as the saturation level of the active component
was calculated to be 2.3121+-0.0964 s, and the Half-life value, which is
required flare total time to reach the saturation, was computed to be 2233.6 s.
In addition, the frequency of N1, which is the number of flares per an hour in
the system, was found to be 0.05087 1/h, while the flare frequency N2 that the
flare-equivalent duration emitting per an hour was found to be 0.00051.
Contrary to the spot activity, it has been found that the flares are in tends
to appear at specific phases due to the white dwarf component.
