The role of non-axisymmetry of magnetic flux rope in constraining solar eruptions

TL;DR

This study uses data-driven MHD simulations to show that the non-axisymmetry of magnetic flux ropes significantly influences whether solar eruptions are successful or failed, emphasizing the importance of flux rope topology.

Contribution

It introduces the role of non-axisymmetry in flux ropes as a key factor in constraining solar eruptions, expanding current models.

Findings

Non-axisymmetry constrains eruption success.

Simulation reproduces observed confined eruption.

Lorentz force component from non-axisymmetry is crucial.

Abstract

Whether a solar eruption is successful or failed depends on the competition between different components of the Lorentz force exerting on the flux rope that drives the eruption. The present models only consider the strapping force generated by the background magnetic field perpendicular to the flux rope and the tension force generated by the field along the flux rope. Using the observed magnetic field on the photosphere as a time-matching bottom boundary, we perform a data-driven magnetohydrodynamic simulation for the 30 January 2015 confined eruption and successfully reproduce the observed solar flare without a coronal mass ejection. Here we show a Lorentz force component, resulting from the radial magnetic field or the non-axisymmetry of the flux rope, which can essentially constrain the eruption. Our finding contributes to the solar eruption model and presents the necessity of considering the topological structure of a flux rope when studying its eruption behaviour.