Compression, Impact and Hot Rebound Flows from Coronal Rain Downflows

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 High-Resolution Imager in Extreme Ultraviolet of Solar Orbiter, the Atmospheric Imaging Assembly of the Solar Dynamics Observatory, and the Slit-Jaw Imager (SJI) from the 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 ≈600~km and densities of ≈5×10¹¹~cm⁻³ are seen to fall with a strong compression ahead. During the compression we measure a low polytropic index with $γ=1.085$, suggesting the presence of molecules. The rain shower carries a total of 3.09×10²⁶~erg, and the clumps produce impacts seen in all EUV channels and in SJI~1400~Å. The impacts generate hot rebound flows with temperatures of 106.2-106.3~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 2.56×10⁻²~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.