Investigating pre-eruptive magnetic properties at the footprints of erupting magnetic flux ropes

Abstract

It is well established that solar eruptions are powered by free magnetic energy stored in current-carrying magnetic field in the corona. It has also been generally accepted that magnetic flux ropes (MFRs) are a critical component of many coronal mass ejections (CMEs). What remains controversial is whether MFRs are present well before the eruption. Our aim is to identify progenitors of MFRs, and investigate pre-eruptive magnetic properties associated with these progenitors. Here we analyze 28 MFRs erupting within 45 deg from the disk center from 2010 to 2015. All MFRs'feet are well identified by conjugate coronal dimmings. We then calculate magnetic properties at the feet of the MFRs, prior to their eruptions, using Helioseismic and Magnetic Imager (HMI) vector magnetograms. Our results show that only 8 erupting MFRs are associated with significant non-neutralized electric currents, 4 of which also exhibit pre-eruptive dimmings at the foot-prints. Twist and current distributions are asymmetric at the two feet of these MFRs. The presence of pre-eruption dimmings associated with non-neutralized currents suggests the pre-existing MFRs. Furthermore, evolution of conjugate dimmings and electric currents within the foot-prints can provide clues about the internal structure of MFRs and their formation mechanism.

40 pages, 13 figures, 6 tables, Accepted for publication in ApJ

References in corpus (10)

• The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: SHARPs -- Space-weather HMI Active Region Patches
• The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance
• Ideal kink instability of a magnetic loop equilibrium
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• Structures of Interplanetary Magnetic Flux Ropes and Comparison with Their Solar Sources
• Electric-Current Neutralization, Magnetic Shear, and Eruptive Activity in Solar Active Regions
• Evolution of the Toroidal Flux of CME Flux Ropes during Eruption
• Gradual Solar Coronal Dimming and Evolution of Coronal Mass Ejection in the Early Phase
• Degree of electric current neutralization and the activity in solar Active Regions
• Electric current evolution at the footpoints of solar eruptions

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