📝 SummarXiv

Abstract

Understanding the processes associated with coronal rain due to the thermal non-equilibrium (TNE) and thermal instability (TI) scenario can help us understand coronal heating. We aim to study the properties of a quiescent coronal rain event and its effect on the solar atmosphere. We utilise space-based data from the \textit{High-Resolution Imager in Extreme Ultraviolet} of Solar Orbiter, the \textit{Atmospheric Imaging Assembly} of the Solar Dynamics Observatory, and the Slit-Jaw Imager (SJI) from the \textit{Interface Region Imaging Spectrograph} from November 1st, 2023. During the coronal rain shower, the coronal loop exhibits large EUV variability and drastic changes in sub-structure. Coronal rain clumps with total velocities between 72~km~s$^{-1}$ and 87~km~s$^{-1}$ and cool EUV absorbing core sizes of $\approx$600~km and densities of $\approx5\times10^{11}$~cm$^{-3}$ are seen to fall with a strong compression ahead. During the compression we measure a low polytropic index with $\gamma=1.085$, suggesting the presence of molecules. The rain shower carries a total of $3.09\times10^{26}$~erg, and the clumps produce impacts seen in all EUV channels and in SJI~1400~\AA. The impacts generate hot rebound flows with temperatures of $10^{6.2}-10^{6.3}~$K and velocities of $85-87$ km~s$^{-1}$, which refill and reheat the loop but carry less than $20\%$ of the clumps' kinetic energies. We find signatures of a steady footpoint heating, in agreement with the TNE-TI scenario, with an estimated amplitude of $2.56\times10^{-2}~$erg~cm$^{-3}$~s$^{-1}$ in agreement with active region estimates. Coronal rain may therefore be a good proxy for the total integrated heating that gives birth to TNE-TI.