Observing the fine structure of loops through high resolution spectroscopic observations of coronal rain with the CRISP instrument at the Swedish Solar Telescope

TL;DR

This study provides high-resolution spectroscopic observations of coronal rain, revealing its properties and role in understanding coronal magnetic fields, thermodynamics, and heating processes in active regions.

Contribution

First high-resolution spectroscopic analysis of coronal rain assessing its dynamics, thermodynamics, and magnetic implications, supporting multi-strand loop models and coronal heating constraints.

Findings

Coronal rain consists of small, dense chromospheric cores with temperatures below 7000 K.

Average falling speed of coronal rain is 70 km/s with accelerations below gravity.

Coronal rain occurs in 7-30% of coronal volume and lasts 5-20 hours in loops.

Abstract

We present here one of the first high resolution spectroscopic observations of coronal rain, performed with the CRISP instrument at the Swedish Solar Telescope. This work constitutes the first attempt to assess the importance of coronal rain in the understanding of the coronal magnetic field in active regions. A large statistical set is obtained in which dynamics (total velocities and accelerations), shapes (lengths and widths), trajectories (angles of fall) and thermodynamic properties (temperatures) of the condensations are derived. Specifically, we find that coronal rain is composed of small and dense chromospheric cores with average widths and lengths of 310 km and 710 km respectively, average temperatures below 7000 K, displaying a broad distribution of falling speeds with an average of 70 km/s and accelerations largely below the effective gravity along loops. Through estimates of the ion-neutral coupling in the blobs we show that coronal rain acts as a tracer of the coronal magnetic field, thus supporting the multi-strand loop scenario, and acts as a probe of the local thermodynamic conditions in loops. We further find that the cooling in neighboring strands occurs simultaneously in general suggesting a similar thermodynamic evolution among strands, which can be explained by a common footpoint heating process. Constraints for coronal heating models of loops are thus provided. Estimates of the fraction of coronal volume with coronal rain give values between 7% and 30%. Estimates of the occurrence time of the phenomenon in loops set times between 5 and 20 hours, implying that coronal rain may be a common phenomenon, in agreement with the frequent observations of cool downflows in EUV lines. The coronal mass drain rate in the form of coronal rain is estimated to be on the order of 5x10^9 g/s, a significant quantity compared to the estimate of mass flux into the corona from spicules.