Coronal Heating with Sweet-Parker Picoflares

Details Coronal Heating with Sweet-Parker Picoflares Coronal Heating with Sweet-Parker Picoflares

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..325..289t&link_type=abstract

The Solar-B Mission and the Forefront of Solar Physics, ASP Conference Series, Vol. 325, Proceedings of the Fifth Solar-B Scienc

Physics

Scientific paper

Katsukawa & Tsuneta (2001) found an excess fluctuation in soft X-rays coming from active regions, and proposed that the fluctuation was attributed to ubiquitous tiny bursts. They estimated the energy range of individual bursts to be 1020--1022 erg. There appears to be a big desert, the void in which no burst occurs for 3--6 orders of magnitudes in energy from the pico-flare range to the observed micro-flare range, indicating that a separate physical mechanism is responsible for the picoflares. We propose that the picoflares are due to Sweet-Parker reconnection, which is presumably easier to occur than the Petschek reconnection responsible for larger flares. We point out the critical importance of the simultaneous observations with SolarB X-ray/EUV and visible-light telescopes.

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