  We report the white light flare rates for 10 ultracool dwarfs (UCDs) using
\textit{Kepler K2} short cadence data. Among our sample stars, two have
spectral type M6, three are M7, three are M8 and two are L0. Most of our
targets are old low mass stars. We identify a total of 283 flares in all of the
stars in our sample, with \textit{Kepler} energies in the range log
\textit{E$_{Kp}$} $\sim$(29 - 33.5) erg. Using the maximum-likelihood method of
line fitting, we find that the flare frequency distribution (FFD) for each star
in our sample follows a power law with slope -$\alpha$ in range -(1.3-2.0). We
find that cooler objects tend to have shallower slopes. For some of our
targets, the FFD follows either a broken power law, or a power law with an
exponential cutoff. For the L0 dwarf 2MASS J12321827-0951502, we find a very
shallow slope (-$\alpha$ $=$ -1.3) in the \textit{Kepler} energy range
(0.82-130)$\times$10$^{30}$ erg: this L0 dwarf has flare rates which are
comparable to the rates of high energy flares in stars of earlier spectral
types. In addition, we report photometry of two superflares: one on the L0
dwarf 2MASS J12321827-0951502 and another on the M7 dwarf 2MASS
J08352366+1029318. In case of 2MASS J12321827-0951502, we report a flare
brightening by a factor of $\sim$144 relative to the quiescent photospheric
level. Likewise, for 2MASS J08352366+1029318, we report a flare brightening by
a factor of $\sim$60 relative to the quiescent photospheric level. These two
superflares have bolometric (UV/optical/infrared) energies 3.6 $\times$
10$^{33}$ erg and 8.9 $\times$ 10$^{33}$ erg respectively, while the FWHM time
scales are very short, $\sim$2 minutes. We find that the M8 star TRAPPIST-1 is
more active than the M8.5 dwarf: 2M03264453+1919309, but less active than
another M8 dwarf (2M12215066-0843197).
