  We study the evolution of a mini-filament eruption in a quiet region at the
center of the solar disk and its impact on the ambient atmosphere. We used
high-spectral resolution imaging spectroscopy in H$\alpha$ acquired by the
echelle spectrograph of the Vacuum Tower Telescope (VTT), Tenerife, Spain,
photospheric magnetic field observations from the Helioseismic and Magnetic
Imager (HMI), and UV/EUV imaging from the Atmospheric Imaging Assembly (AIA) of
the Solar Dynamics Observatory (SDO). The H$\alpha$ line profiles were
noise-stripped using Principal Component Analysis (PCA) and then inverted to
produce physical and cloud model parameter maps. The minifilament formed
between small-scale, opposite-polarity magnetic features through a series of
small reconnection events and it erupted within an hour after its appearance in
H$\alpha$. Its development and eruption exhibited similarities with large-scale
erupting filaments, indicating the action of common mechanisms. Its eruption
took place in two phases, namely a slow rise and a fast expansion, and it
produced a coronal dimming, before the minifilament disappeared. During its
eruption we detected a complicated velocity pattern, indicative of a twisted,
thread-like structure. Part of its material returned to the chromosphere
producing observable effects on nearby low-lying magnetic structures. Cloud
model analysis showed that the minifilament was initially similar to other
chromospheric fine structures, in terms of optical depth, source function and
Doppler width, but it resembled a large-scale filament on its course to
eruption. High spectral resolution observations of the chromosphere can provide
a wealth of information regarding the dynamics and properties of minifilaments
and their interactions with the surrounding atmosphere.
