On 1 Oct 2011 two coronal mass ejections (CMEs) erupted from neighbouring active regions and each generated a coronal shock that excited a distinct type‑II burst in the 180–25 MHz band. The first burst (09:06–09:12 UT) drifted at 0.3 MHz s⁻¹, travelled 1.28–1.89 R⊙ and moved at 1 701–2 163 km s⁻¹. Its radio sources lay on the shock nose-front. The second burst (09:55–09:57 UT) drifted faster, at 0.6 MHz s⁻¹, travelled 1.31–1.65 R⊙ and moved at 1 282–1 651 km s⁻¹, with sources positioned on the shock flank. The study combined NRH radio imaging at 228, 173.2 and 150.9 MHz, EUV observations from SDO/AIA, and white‑light coronagraph data from STEREO and SOHO/LASCO. Using heliocentric deprojection and 3‑D Monte Carlo ray‑tracing, the team corrected for line‑of‑sight projection and scattering by solar turbulence, finding that the centroids of the radio bursts trace the expanding flanks of 3‑D shock bubbles. Because the analysis relied on line‑of‑sight observations, the derived positions and speeds represent apparent values; high‑frequency imaging above 180 MHz was not available, and projection and scattering still influence the results.