  We observed a C-class flare at the outer boundary of the super-penumbra of a
sunspot. The flare was triggered by an emerging magnetic bipolar region that
was obliquely oriented with respect to the super-penumbral fibrils. The flare
started due to the low height magnetic reconnection of emerging magnetic flux
with super-penumbral field resulting hot multi-temperature plasma flows in the
inverse Evershed flow channel and its overlying atmosphere. The inverse
Evershed flows in the chromosphere start from super penumbra towards sunspot
that end at the outer boundary of the penumbra. The hot plasma flow towards the
sunspot in the inverse Evershed channels show about 10 km s$^{-1}$ higher
velocity in H$\alpha$ wavelengths compared to the plasma emissions at various
temperatures as seen in different AIA filters. Even though these velocities are
about seven times higher than the typical inverse-Evershed flow speeds, the
flow is diminished at the outer boundary of the sunspot's penumbra. This
suggests that the super-penumbral field lines that carry the inverse Evershed
flows, are discontinued at the boundary where the penumbral field lines dive
into the sun and these two sets of field lines are completely distinct. The
discontinuity in the typical magnetic field and plasma properties at the
adjoining of these two sets of field lines further leads the discontinuity in
the characteristic magnetoacoustic and Alfv\'en speeds, therefore, stopping the
plasma flows further on. The multi-temperature plasma in the inverse Evershed
channels exhibits \textbf{possible} longitudinal oscillations initially during
the onset of the flare, and later flows towards the sunspot. In the
multi-temperature view, the different layers above the flare region have the
mixture of supersonic as well as subsonic flows.
