From coronal observations to MHD simulations, the building blocks for 3D models of solar flares

TL;DR

This paper reviews the development of 3D numerical simulations of solar flares, linking observations with models to understand energy release and magnetic field evolution, crucial for space weather prediction.

Contribution

It introduces recent advances in 3D MHD simulations of solar flares, integrating observational data with modeling to elucidate eruption mechanisms.

Findings

Simulations reproduce observed flare features

Models predict magnetic field evolution

Observational data supports eruption mechanisms

Abstract

Solar flares are energetic events taking place in the Sun's atmosphere, and their effects can greatly impact the environment of the surrounding planets. In particular, eruptive flares, as opposed to confined flares, launch coronal mass ejections into the interplanetary medium, and as such, are one of the main drivers of space weather. After briefly reviewing the main characteristics of solar flares, we summarize the processes that can account for the build up and release of energy during their evolution. In particular, we focus on the development of recent 3D numerical simulations that explain many of the observed flare features. These simulations can also provide predictions of the dynamical evolution of coronal and photospheric magnetic field. Here we present a few observational examples that, together with numerical modelling, point to the underlying physical mechanisms of the eruptions.