  Intermediate stages between pores and sunspots are a rare phenomenon and can
manifest with the formation of transient photospheric penumbral-like filaments.
Although the magnetic field changes rapidly during the evolution of such
filaments, they have not been shown to be connected to magnetic reconnection
events yet. We analyzed observations of a pore in NOAA AR 12739 from the
Swedish Solar Telescope including spectropolarimetric data of the Fe I 6173
{\AA} and the Ca II 8542 {\AA} line and spectroscopic data of the Ca II K 3934
{\AA} line. The VFISV Milne-Eddington inversion code and the multi-line Non-LTE
inversion code STiC were utilized to obtain atmospheric parameters in the
photosphere and the chromosphere. Multiple filamentary structures of inclined
magnetic fields are found in photospheric inclination maps at the boundary of
the pore, although the pore never developed a penumbra. One of the filaments
shows a clear counterpart in continuum intensity maps in addition to
photospheric blueshifts. During its decay, a brightening in the blue wing of
the Ca II 8542 {\AA} line is observed. The Ca II K 3934 {\AA} and the Ca II
8542 {\AA} lines show complex spectral profiles in this region. Depth-dependent
STiC inversion results using data from all available lines yield a temperature
increase (roughly 1000 Kelvin) and bidirectional flows (magnitudes up to 8
km/s) at log tau=-3.5. The temporal and spatial correlation of the decaying
filament (observed in the photosphere) to the temperature increase and the
bidirectional flows in the high photosphere/low chromosphere suggests that they
are connected. We propose scenarios in which magnetic reconnection happens at
the edge of a rising magnetic flux tube in the photosphere. This leads to both
the decay of the filament in the photosphere and the observed temperature
increase and the bidirectional flows in the high photosphere/low chromosphere.
