Coronal Rain in Randomly Heated Arcades

Adopting the MPI-AMRVAC code, we present a 2.5-dimensional magnetohydrodynamic (MHD) simulation, which includes thermal conduction and radiative cooling, to investigate formation evolution of coronal rain phenomenon. We perform simulation in initially linear force-free magnetic fields host chromospheric, transition region, plasma, with turbulent heating localized on their footpoints. Due instability, condensations start occur at loop top, rebound shocks are generated by siphon inflows. Condensations fragment into smaller blobs moving downwards as they hit lower atmosphere, concurrent upflows triggered. Larger clumps show us clear "coronal showers" dark structures synthetic EUV hot channels bright cool cores 304 {\AA} channel, well resembling real observations. Following dynamics for more than 10 hours, carry out statistical study all quantify widths, lengths, areas, velocity distributions, other properties. The shows continuous heating-condensation cycles, cycles emissions. Compared previous studies adopting steady heating, happens faster erratic cycles. Although most falling downward, upward-moving exist basically every moment. also track movement individual forces driving movements. have prominence-corona transition-region-like structure surrounding them, movements dominated pressure very dynamic system.