  The present study investigates a mini-filament eruption associated with
cancelling magnetic fluxes. The eruption originates from a small-scale loop
complex commonly known as a Coronal Bright Point (CBP). The event is uniquely
recorded in both the imaging and spectroscopic data taken with IRIS. We analyse
IRIS spectroscopic and slit-jaw imaging observations as well as images taken in
the extreme-ultraviolet channels of AIA, and line-of-sight magnetic-field data
from HMI onboard the SDO. We also employ an NLFFF relaxation approach based on
the HMI magnetogram time series. We identify a strong small-scale brightening
as a micro-flare in a CBP. The mini-eruption manifests with the ejection of hot
(CBP loops) and cool (mini-filament) plasma recorded in both the imaging and
spectroscopic data. The micro-flare is preceded by the appearance of an
elongated bright feature in the IRIS slit-jaw 1400 A images located above the
polarity inversion line. The micro-flare starts with an IRIS pixel size
brightening and propagates bi-directionally along the elongated feature. We
detect in both the spectral and imaging IRIS data and AIA data, strong flows
along and at the edges of the elongated feature which we believe represent
reconnection outflows. Both edges of the elongated feature that wrap around the
edges of the erupting MF evolve into a J-type shape creating a sigmoid
appearance. A quasi-separatrix layer (QSL) is identified in the vicinity of the
polarity inversion line by computing the squashing factor Q in different
horizontal planes of the NLFFF model. The QSL reconnection site has the same
spectral appearance as the so-called explosive events identified by strong
blue- and red-shifted emission, thus answering a long outstanding question
about the true nature of this spectral phenomenon.

Solar and Stellar Astrophysics