Magnetic topology and related coronal rain flows near the source region of sunspot supersonic downflows. (a) Reconstructed magnetic topology from the PFSS model. (b) Observed morphological topology in EUVI 195 Å running-difference image at around 09:35 UT. The solar disk and the FOV of these images are shown as the white circle and the green rectangle, respectively. “L1” denotes the upward-moving coronal loops from the X-shaped structure. Near the left feet of “L1”, a weak brightening signal was observed. (c) EUVI 195 Å running-difference image and (d) 304 Å image (panel d, using reversed color table) taken at 09:56 UT. The FOV of panels c and d is shown as the dashed-line rectangle in panel b. The coronal rain and the X-shaped structure below the dip are marked by the arrows. The dashed lines outline the possible magnetic field geometry. An animation showing the temporal evolution of panels c and d from 02:00−12:55 UT is available online.