Observations of Reconnection Flows in a Flare on the Solar Disk

29 Aug 2017Juntao WangP. J. A. SimoesN. L. S. JeffreyL. FletcherP. J. WrightI. G. Hannah

Magnetic reconnection is a well-accepted part of the theory of solar eruptive events, though the evidence is still circumstantial. Intrinsic to the reconnection picture of a solar eruptive event, particularly in the standard model for two-ribbon flares ("CSHKP" model), are an advective flow of magnetized plasma into the reconnection region, expansion of field above the reconnection region as a flux rope erupts, retraction of heated post-reconnection loops, and downflows of cooling plasma along those loops... (read more)

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