  On 2014 October 30, a band-splitted type II radio burst associated with a
coronal mass ejection (CME) observed by the Atmospheric Imaging Assembly (AIA)
on board the Solar Dynamic Observatory (SDO) occurred over the southeast limb
of the Sun. The fast expansion in all directions of the plasma front acted as a
piston and drove a spherical fast shock ahead of it, whose outward progression
was traced by simultaneous images obtained with the Nan\c{c}ay Radioheliograph
(NRH). The geometry of the CME/shock event was recovered through 3D modeling,
given the absence of concomitant stereoscopic observations, and assuming that
the band-splitted type II burst was emitted at the intersection of the shock
surface with two adjacent low-Alfven speed coronal streamers. From the derived
spatiotemporal evolution of the standoff distance between shock and CME leading
edge, we were finally able to infer the magnetic field strength $B$ in the
inner corona. A simple radial profile of the form $B(r) = (12.6 \pm 2.5)
r^{-4}$ nicely fits our results, together with previous estimates, in the range
$r = 1.1-2.0$ solar radii.
