The Role of Magnetic Reconnection in the Formation of Transequatorial Loops

Details The Role of Magnetic Reconnection in the Formation of Transequatorial Loops The Role of Magnetic Reconnection in the Formation of Transequatorial Loops

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.1002m&link_type=abstract

American Astronomical Society, SPD meeting #34, #10.02; Bulletin of the American Astronomical Society, Vol. 35, p.825

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Transequatorial loops often bridge large regions of very small field strength in which no emergence other than that of tiny dipoles is observed. It is very unlikely on theoretical grounds, and has never been observed, that such loops emerge as pre-existing flux tubes from below the chromosphere. Moreover, of the two active regions that these loops connect one is usually demonstrably older than the other, so that a loop connecting them could not have emerged with the older one, because it would have had nowhere to connect to. Taken together this is nearly indisputable evidence of reconnection in the corona.
I will review a number of recently published observations that support the statements above, and consider the implications for dynamo models from the coronal formation of transequatorial loops

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