  The focus of this investigation is to quantify the conversion of magnetic to
thermal energy initiated by a quiet Sun cancellation event and to explore the
resulting dynamics from the interaction of the opposite polarity magnetic
features. We used imaging spectroscopy in the H$\alpha$ line, along with
spectropolarimetry in the \ion{Fe}{I} 6173~{\AA} and \ion{Ca}{II} 8542~{\AA}
lines from the Swedish Solar Telescope (SST) to study a reconnection-related
cancellation and the appearance of a quiet Sun Ellerman bomb (QSEB). We
observed, for the first time, QSEB signature in both the wings and core of the
\ion{Fe}{I} 6173~{\AA} line. We also found that, at times, the \ion{Fe}{I}
line-core intensity reaches higher values than the quiet Sun continuum
intensity. From FIRTEZ-dz inversions of the Stokes profiles in \ion{Fe}{I} and
\ion{Ca}{II} lines, we found enhanced temperature, with respect to the quiet
Sun values, at the photospheric ($\log\tau_c$ = -1.5; $\sim$1000 K) and lower
chromospheric heights ($\log\tau_c$ = -4.5; $\sim$360 K). From the calculation
of total magnetic energy and thermal energy within these two layers it was
confirmed that the magnetic energy released during the flux cancellation can
support heating in the aforesaid height range. Further, the temperature
stratification maps enabled us to identify cumulative effects of successive
reconnection on temperature pattern, including recurring temperature
enhancements. Similarly, Doppler velocity stratification maps revealed impacts
on plasma flow pattern, such as a sudden change in the flow direction.
