  The radial speed of a coronal mass ejection (CME) determines the
shock-driving capability of a CME as indicated by the presence of a type II
radio burst. Here we report on the April 18, 2014 CME that was associated with
a type II radio burst in the metric and interplanetary domains. We used the
radio-burst data provided by the San Vito Solar Observatory of the Radio Solar
Telescope Network and data from the Wind spacecraft. The CME is a full halo in
the field of view of the coronagraphs on board the Solar and Heliospheric
Observatory (SOHO). The CME was also observed by the coronagraphs on board the
Solar Terrestrial Relations Observatory (STEREO). We computed the CME shock and
flux rope speeds based on the multi-view observations by the different
coronagraphs and by EUV instruments. We determined the shock speed from metric
and interplanetary radio observations and found them to be consistent with
white-light observations, provided the metric type II burst and its
continuation into the decameter-hectometric domain are produced at the shock
flanks, where the speed is still high enough to accelerate electrons that
produce the type II bursts. Interestingly, there was an interplanetary type II
burst segment consistent with an origin at the shock nose suggesting that the
curved shock was crossing plasma levels separated by a few solar radii. We
conclude that the CME speed is high enough to produce the interplanetary Type
II burst and a solar energetic particle (SEP) event. However, the speed is not
high enough to produce a ground level enhancement (GLE) event, which requires
the shock to form at a height of ~1.5 Rs.
