Multidimensional modeling of coronal rain dynamics

TL;DR

This paper presents the first multidimensional magnetohydrodynamic simulations of coronal rain, revealing detailed formation, dynamics, and interactions of blobs that match observational data, advancing understanding of coronal heating.

Contribution

It introduces the first multidimensional MHD simulations capturing coronal rain formation and evolution, providing new insights into blob dynamics and their relation to coronal heating.

Findings

Blob widths and velocities match observations.

Blob deformation into V-shapes observed.

In situ evaporation and siphoning of blobs demonstrated.

Abstract

We present the first multidimensional, magnetohydrodynamic simulations which capture the initial formation and the long-term sustainment of the enigmatic coronal rain phenomenon. We demonstrate how thermal instability can induce a spectacular display of in-situ forming blob-like condensations which then start their intimate ballet on top of initially linear force-free arcades. Our magnetic arcades host chromospheric, transition region, and coronal plasma. Following coronal rain dynamics for over 80 minutes physical time, we collect enough statistics to quantify blob widths, lengths, velocity distributions, and other characteristics which directly match with modern observational knowledge. Our virtual coronal rain displays the deformation of blobs into $V$-shaped like features, interactions of blobs due to mostly pressure-mediated levitations, and gives the first views on blobs which evaporate in situ, or get siphoned over the apex of the background arcade. Our simulations pave the way for systematic surveys of coronal rain showers in true multidimensional settings, to connect parametrized heating prescriptions with rain statistics, ultimately allowing to quantify the coronal heating input.