  Using the observations from Solar Dynamics Observatory, we study an eruption
of a hot-channel flux rope (FR) near the solar-limb on February 9, 2015. The
pre-eruptive structure is visible mainly in EUV 131 $\mathring{\mathrm{A}}$
images with two highly-sheared loop structures. They undergo slow rise motion
and then reconnect to form an eruptive hot-channel as in the tether-cutting
reconnection model. The J-shaped flare-ribbons trace the footpoint of the FR
which is identified as the hot-channel. Initially, the hot channel is observed
to rise slowly at 40 km s$^{-1}$, followed by an exponential rise from 22:55 UT
at a coronal height of 87$\pm$2 Mm. Following the onset of the eruption at
23:00 UT, the flare-reconnection adds to the acceleration process of the CME
within 3 R$_\odot$. Later on, the CME continues to accelerate at 8 m s$^{-2}$
during its propagation period. Further, the eruption launched type-II followed
by III, IVm radio bursts. The start and end times of type-IVm correspond to the
CME core height of 1.5 and 6.1 R$_\odot$, respectively. Also the spectral index
is negative suggesting the non-thermal electrons trapped in the closed loop
structure. Accompanied with type-IVm, this event is unique in the sense that
the flare ribbons are very clearly observed along with the erupting hot
channel, which strongly supports that the hooked-part of J-shaped flare ribbons
outlines the boundary of the erupting FR.
