  We study the early evolution of a hot-channel-like magnetic flux rope (MFR)
toward eruption. Combining with imaging observation and magnetic field
extrapolation, we find that the hot channel possibly originated from a
pre-existing seed MFR with a hyperbolic flux tube (HFT). In the precursor
phase, three-dimensional tether-cutting reconnection at the HFT is most likely
resulting in the heating and buildup of the hot channel. In this process, the
forming hot channel was rapidly enlarged at its spatial size and slipped its
feet to two remote positions. Afterward, it instantly erupted outwards with an
exponential acceleration, leaving two core dimmings near its feet. We suggest
that pre-flare reconnection at the HFT played a crucial role in enlarging the
seed MFR and facilitating the onset of its final solar eruption. Moreover, a
recently predicted drifting of MFR's footpoints was detected at both core
dimmings. In particular, we find that MFR's west footpoint drift was induced by
a new reconnection geometry among the erupting MFR's leg and thereby inclined
arcades. As MFR's west footpoints gradually drifted to a new position, a set of
newborn atypical flare loops connected into the west core dimming, causing a
rapid decrease of dimmed area inside this core dimming and also generating a
secondary flare ribbon at their remote feet. This reveals that core dimmings
may suffer a pronounced diminishment due to the eruptive MFR's footpoint drift,
implying that mapping the real footpoints of the erupting MFR down to the Sun's
surface is more difficult than previously thought.
