Data-constrained Magnetohydrodynamic Simulation of an Intermediate Solar Filament Eruption

TL;DR

This paper presents a data-constrained MHD simulation method for modeling large-scale solar filament eruptions in weak magnetic field regions, successfully reproducing eruption dynamics and flare evolution.

Contribution

It introduces a flux rope embedding technique combined with a nonlinear force-free field and MHD simulation for global-scale solar eruptions.

Findings

Successfully simulated an M8.7 solar flare eruption.

Reproduced flare ribbon evolution and flux rope kinematics.

Demonstrated potential for modeling large-scale eruptions from weak magnetic fields.

Abstract

Solar eruptive activities could occur in weak magnetic field environments and over large spatial scales, especially relevant to eruptions involving intermediate or quiescent solar filaments. To handle the large scales, we implement and apply a flux rope embedding method using regularized Biot-Savart laws in the spherical coordinate system. Combined with a potential field source surface model and a magneto-frictional method, a nonlinear force-free field comprising a flux rope embedded in a potential field is constructed. Using the combined nonlinear force-free field as the initial condition, we then perform a zero-$\beta$ data-constrained magnetohydrodynamic (MHD) simulation for an M8.7 flare at 03:38 UT on 2012 January 23. The MHD model reproduces the eruption process, flare ribbon evolution (represented by the quasi-separatrix layer evolution) and kinematics of the flux rope. This approach could potentially model global-scale eruptions from weak field regions.