Implications of spicule activity on coronal loop heating and catastrophic cooling

We report on the properties of coronal loop foot-point heating with observations at highest resolution, from CRisp Imaging Spectro-Polarimeter (CRISP) located Swedish 1-m Solar Telescope (SST) and co-aligned NASA Dynamics Observatory (SDO) observations, Type II spicules in chromosphere their signatures EUV corona. Here, we address one important issue, as to why there is not always a one-to-one correspondence, between hot plasma signatures, i.e. beyond TR temperatures. do detect any difference spectral quiet Sun region compared dominated by loops. On other hand, number density close foot-points active found be an order magnitude higher than case. A differential emission measure analysis reveals peak $\sim 5 \times 10^5$ K 10$^{22}$~cm$^{-5}$~K$^{-1}$. Using this result constraint, conduct numerical simulations show that energy input $1.25 10^{24}$ erg (corresponding $\sim$10 RBEs contributing burst) manage reproduce observation very closely. However, simulation runs lower thermal synthetic AIA $171 {\AA}$ indicating critical required account for $171{\AA}$ simulation. Furthermore, ($1.25 ergs) catastrophic cooling cycle duration $\sim$5 hours, matching periodicity observe observations.