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.
Highlights
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
Magnetic flux ropes (MFRs) can erupt under some conditions, which can in turn drive prominence eruptions and coronal mass ejections (CMEs)[16], as well as solar flares when magnetic reconnection occurs[17]
We focus on the intense M2.0 flare (Fig. 1) that occurred at 00:32 UT on 30 January 2015, which was observed by the Atmospheric Imaging Assembly[35] (AIA) on board Solar Dynamics Observatory[36] (SDO)
Summary
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. 1234567890():,; Magnetic flux ropes (MFRs) are a bundle of twisted field lines with electric currents flowing inside. They play a critical role in explaining a variety of phenomena in astrophysics[1], solar physics[2,3,4,5], space physics[6], and laboratory plasmas[7]. MFRs can erupt under some conditions, which can in turn drive prominence eruptions and coronal mass ejections (CMEs)[16], as well as solar flares when magnetic reconnection occurs[17].
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