  We wrote and used an automated flare detection Python script to search for
super-flares on main-sequence stars of types A, F, G, K, and M in Kepler's
long-cadence data from Q0 to Q17. We studied the statistical properties of the
occurrence rate of super-flares. For the G-type data set, we compared our
results with the previous results of Okamoto et al. 2021 by splitting the data
set into four rotational bands. We found similar power law indices for the
flare frequency distribution. Hence, we show that inclusion of high-pass
filter, sample biases, gyrochronology and completeness of flare detection is of
no significance, as our results are similar to Okamoto et al. 2021. We
estimated that a super-flare on G-type dwarfs of energy of $10^{35}$ erg occurs
on a star once every 4360 years. We found 4637 super-flares on 1896 G-type
dwarfs. Moreover, we found 321, 1125, 4538 and 5445 super-flares on 136, 522,
770 and 312 dwarfs of types A, F, K and M, respectively. We found that the
occurrence rate ($dN/dE$) of super-flares versus flare energy, $E$, shows a
power-law distribution with $dN/dE \propto E^{-\alpha}$, where $\alpha \simeq$
2.0 to 2.1 for the spectral types from F-type to M-type stars. In contrast, the
obtained $\alpha \simeq$ 1.3 for A-type stars suggests that the flare
conditions differ from the rest spectral-type stars. We note an increase in
flare incidence rate in F-type to M-type stars and a decrease in A-type to
F-type stars.
