  We report on a multi-wavelength analysis of the 26 January 2014 solar
eruption involving a coronal mass ejection (CME) and a Type-II radio burst,
performed by combining data from various space-and ground-based instruments. An
increasing standoff distance with height shows the presence of a strong shock,
which further manifests itself in the continuation of the metric Type-II burst
into the decameter-hectometric (DH) domain. A plot of speed versus position
angle (PA) shows different points on the CME leading edge travelled with
different speeds. From the starting frequency of the Type-II burst and
white-light data, we find that the shock signature producing the Type-II burst
might be coming from the flanks of the CME. Measuring the speeds of the CME
flanks, we find the southern flank to be at a higher speed than the northern
flank; further the radio contours from Type-II imaging data showed that the
burst source was coming from the southern flank of the CME. From the standoff
distance at the CME nose, we find that the local Alfven speed is close to the
white-light shock speed, thus causing the Mach number to be small there. Also,
the presence of a streamer near the southern flank appears to have provided
additional favorable conditions for the generation of shock-associated radio
emission. These results provide conclusive evidence that the Type-II emission
could originate from the flanks of the CME, which in our study is from the the
southern flank of the CME.
