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J. Qiu (BBSO/NJIT)
I will discuss the observational relationship among magnetic reconnection, flare emission, and the rising motion of the erupting flux ropes derived from several well-observed solar eruptive events. The role of magnetic reconnection in the process of coronal mass ejections (CMEs) remains an issue in heated debate. Very recently, some observations and numerical simulations suggested that fast acceleration of CMEs takes place in the early stage of flux rope eruption, which coincides with the impulsive phase of the flare. We furthered such studies by measuring the rate of magnetic reconnection from flare observations and comparing it with the evolution of erupting flux ropes. The study verifies that the reconnection rate in the low corona is temporally correlated with the flare non-thermal emission, and more importantly, with acceleration of erupting flux ropes in the low corona. The structures of flux ropes, represented by erupting filaments and CMEs at 2-30 solar radii, and their magnetic configurations are also discussed.
The author(s) of this abstract have provided an email address for comments about the abstract: qiuj@bbso.njit.edu
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Bulletin of the American Astronomical Society, 36 #2
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