  We present a multi-wavelength analysis of the eruption of a hot coronal
channel associated with an X1.0 flare (SOL2013-10-28T02:03) from the active
region NOAA 11875 by combining observations from AIA/SDO, HMI/SDO, RHESSI, and
HiRAS. EUV images at high coronal temperatures indicated the presence of a hot
channel at the core of the active region from the early pre-flare phase
evidencing the pre-existence of a quasi-stable magnetic flux rope. The hot
channel underwent an activation phase after a localized and prolonged pre-flare
event occurring adjacent to one of its footpoints. Subsequently, the flux rope
continued to rise slowly for $\approx$16 min during which soft X-ray flux
gradually built-up characterizing a distinct precursor phase. The flux rope
transitioned from the state of slow rise to the eruptive motion with the onset
of the impulsive phase of the X1.0 flare. The eruptive expansion of the hot
channel is accompanied by a series of type III radio bursts in association with
impulsive rise of strong hard X-ray non-thermal emissions that included
explicit hard X-ray sources of energies up to $\approx$50 keV from the coronal
loops and $\approx$100 keV from their footpoint locations. Our study contains
evidence that pre-flare activity occurring within the spatial extent of a
stable flux rope can destabilize it toward eruption. Moreover, sudden
transition of the flux rope from the state of slow rise to fast acceleration
precisely bifurcated the precursor and the impulsive phases of the flare which
points toward a feedback relationship between early CME dynamics and the
strength of the large-scale magnetic reconnection.
