<p>Solar type II radio bursts are associated with shock waves driven by coronal mass ejection (CME). Their shapes in the solar radio dynamic spectrum depend on the shock velocity and the electron density traversed by their radio sources. This study examines a stationary type II radio burst. By analyzing observations from the Daocheng Solar Radio Telescope and the Solar Dynamics Observatory/Atmospheric Imaging Assembly, we aim to determine the spatial relationship between type II burst sources and shock fronts. Observations suggest that the radio sources are located in the interaction region between the CME shocks and the coronal streamer. Extensive analysis of their fine structures, particularly the type II herringbones, shows that the radio sources are generally distributed in a frequency order from downstream to upstream regions of the shocks, or only in the upstream region. The observations confirm the existence of type II bursts and associated energetic electrons in the regions upstream and downstream of a shock wave.</p>