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During eruptive solar flares and coronal mass ejections, a non-potential magnetic arcade with much excess magnetic energy goes unstable and reconnects. It produces a twisted erupting flux rope and leaves behind a sheared arcade of hot coronal loops. We suggest that the twist of the erupting flux rope can be determined from conservation of magnetic flux and magnetic helicity and equipartition of magnetic...
We analyzed how sensitivity and accuracy in solar magnetic field measurements may affect the values of mean current helicity density h c and twist parameter α av by comparing these values obtained from two magnetographs (SMFT at Beijing and SFT at Mitaka, Tokyo). When we computed the helicity parameters from the SFT data, we replaced the values...
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