Authors: Felix N. Minta (UT- San Antonio, SwRI), George C. Ho (SwRi, UT- San Antonio), Heather A. Elliott (

We present a multi-diagnostic study of a band-splitting type II solar radio burst observed on 2025 December 04 using observations from the Mingantu Ultrawide Spectral Radioheliograph (MUSER) and the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory. We found the source location of lower-frequency band (LFB) and upper-frequency band (UFB) pairs were separated ~ 127.7 ± 47.7 Mm, ranging from 66.7 to 304.5 Mm. The separation vector is significantly dominated by the tangential component, with a mean offset of 169.3 arcsec compared to the radial offset of only 11.2 arcsec. Our analysis further shows that the dynamic spectrum is deflected at ~ 81°, with the source migrating nearly perpendicular to the radial direction at a transverse speed of ∼458 km/s within 1.2–1.4 R_⊙. These results suggest that LFB and UFB emissions do not originate from colocated regions or from a simple upstream-downstream mechanism. Instead, they arise from spatially distinct regions along a curved, deflected shock flank, and inhomogeneous coronal environment.