Data-driven Radiative Magnetohydrodynamics Simulations with the MURaM Code: the Emergence of Active Region 11158 and the X2.2 Flare

TL;DR

This study uses data-driven radiative MHD simulations with the MURaM code to model active region 11158, successfully reproducing key features of the 2011 X2.2 solar flare, including flux rope eruption, flare ribbons, and shock waves.

Contribution

The paper refines a hybrid modeling strategy to simulate the emergence and eruption of an active region, demonstrating realistic reproduction of observed flare phenomena.

Findings

Simulated flux rope eruption occurred within 3 hours of the actual flare.

The simulation produced flare ribbons and energy deposition consistent with observations.

Reproduced a fast-propagating chromospheric Moreton wave associated with the eruption.

Abstract

We present the application of the data-driven branch of the MURaM code to the extensively studied flare-productive active region 11158. We refine the hybrid model strategy, which was described in the earlier paper of this series, to model the emergence of the active region during 4 solar days starting shortly before 2011 February 11 and the eruption of an X2.2 flare on February 15. After 4 days of evolution, a major eruption of a magnetic flux rope occurs in the simulation at approximately 3 hours (3\% difference) before the real flare. The eruption leads to magnetic reconnection that contributes to bulk heating in the chromosphere and corona. The deposition of flare energy in the chromosphere causes strong condensations and evaporations, which fill hot post-flare loops and bright flare ribbons that exhibit separation and extension similar to the observed ribbon evolution. The synthesized soft X-ray flux corresponds to X class, which is close to the real event. The upward eruption of the flux rope leads to a piston-driven shock and horizontal expansion that exerts a strong downward impact on the lower atmosphere and generate an apparently fast-propagating chromospheric Moreton wave. We conclude that the data-driven radiative simulation of this active region can reproduce the key observational results of the real flare and demonstrate the great potential of this method for studying solar eruptions in a realistic corona environment.