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We present a multi-wavelength analysis of the eruption of a hot coronalchannel associated with an X1.0 flare (SOL2013-10-28T02:03) from the activeregion NOAA 11875 by combining observations from AIA/SDO, HMI/SDO, RHESSI, andHiRAS. EUV images at high coronal temperatures indicated the presence of a hotchannel at the core of the active region from the early pre-flare phaseevidencing the pre-existence of a quasi-stable magnetic flux rope. The hotchannel underwent an activation phase after a localized and prolonged pre-flareevent occurring adjacent to one of its footpoints. Subsequently, the flux ropecontinued to rise slowly for $\approx$16 min during which soft X-ray fluxgradually built-up characterizing a distinct precursor phase. The flux ropetransitioned from the state of slow rise to the eruptive motion with the onsetof the impulsive phase of the X1.0 flare. The eruptive expansion of the hotchannel is accompanied by a series of type III radio bursts in association withimpulsive rise of strong hard X-ray non-thermal emissions that includedexplicit hard X-ray sources of energies up to $\approx$50 keV from the coronalloops and $\approx$100 keV from their footpoint locations. Our study containsevidence that pre-flare activity occurring within the spatial extent of astable flux rope can destabilize it toward eruption. Moreover, suddentransition of the flux rope from the state of slow rise to fast accelerationprecisely bifurcated the precursor and the impulsive phases of the flare whichpoints toward a feedback relationship between early CME dynamics and thestrength of the large-scale magnetic reconnection.

Pre-flare processes, flux rope activation, large-scale eruption and associated X-class flare from the active region NOAA 11875