  We analyse an absorption event within the H$\alpha$ line wings, identified as
a surge, and the co-spatial evolution of an EUV brightening, with spatial and
temporal scales analogous to a small blinker. We conduct a multi-wavelength,
multi-instrument analysis using high-cadence, high-resolution data, collected
by the Interferometric BIdimensional Spectrometer on the Dunn Solar Telescope,
as well as the space-borne Atmospheric Imaging Assembly and Helioseismic and
Magnetic Imager instruments onboard the Solar Dynamics Observatory. One large
absorption event situated within the plage region trailing the lead sunspot of
AR 11579 is identified within the H-alpha line wings. This event is found to be
co-spatially linked to a medium-scale (around 4 arcseconds in diameter)
brightening within the transition region and corona. This ejection appears to
have a parabolic evolution, first forming in the H-alpha blue wing before
fading and reappearing in the H-alpha red wing, and comprises of a number of
smaller fibril events. The line-of-sight photospheric magnetic field shows no
evidence of cancellation leading to this event. Our research has identified
clear evidence that at least a subset of transient brightening events in the
transition region are linked to the influx of cooler plasma from the lower
solar atmosphere during large eruptive events, such as surges. These
observations agree with previous numerical researches on the nature of blinkers
and, therefore, suggest that magnetic reconnection is the driver of the
analysed surge events; however, further research is required to confirm this.
