Rado imaging of the interaction bewteen an coronal mass ejection and nearby coronal structures

Type II solar radio bursts are key tracers of shock waves driven by coronal mass ejections (CMEs), but identifying the precise location of the radio emission source along the extended shock front remains a major challenge. In the presented work, we investigate the origin of two successive, multi-lane metric Type II bursts observed on 16 February 2024. We utilize the novel radio imaging capabilities of the DAocheng Solar Radio Telescope (DART) in conjunction with white-light and EUV coronal observations from the Advanced Space-based Solar Observatory (ASO-S) and the Solar Dynamics Observatory (SDO). The initial Type II burst is imaged ahead of the erupting hot flux rope that develops into the CME. As the CME expands, a second, stronger Type II burst with two distinct emission lanes is detected. Our radio imaging analysis with DART unambiguously pinpoints the sources of these two lanes to the northern and southern flanks of the CME. Crucially, these sources correspond spatially and temporally to the interaction regions between the CME-driven shock and adjacent, dense coronal streamers. The significant enhancement of the radio emission at these locations provides direct evidence that shock-streamer interactions amplify the efficiency of particle acceleration. These observations demonstrate that different lanes in a multi-lane burst can originate from physically distinct regions along a non-uniform, rippled shock front, offering vital constraints on theories of particle energization in the solar corona and inner heliosphere.