The Eruption from a Sigmoid Active Region on 2005 May 13

Details The Eruption from a Sigmoid Active Region on 2005 May 13 The Eruption from a Sigmoid Active Region on 2005 May 13

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0821l&link_type=abstract

American Astronomical Society, SPD meeting #37, #8.21; Bulletin of the American Astronomical Society, Vol. 38, p.234

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A sigmoidal structure of active regions has been of interest as is believed to lead to magnetic eruption. We found from TRACE EUV images that NOAA AR 10759 exhibited a typical sigmoid shape just before the M8.0 flare and a fast halo CME on 2005 May 13, and reduced to a more confined arcade after the eruption. We have thus examined these time dependent changes during the flare by utilizing a multiwavelength data set: EUV (TRACE, EIT), soft X-rays (SXI), H-alpha (BBSO,ISOON), radio spectra (OVSA, Potsdam-Tremsdorf, GBSRBS, Phoenix, RSTN), and CME (LASCO). Several similarities of this event with the runaway tether-cutting scenario elaborated by Moore et al. (2001) has been found. Before the maximum phase, the flare brightening first occurred in the core of the active region, and then two elbows in the outer region gradually expanded, which we compare to the tether-cutting in the sigmoid center and the ejective eruption, respectively. At the flare maximum, the large-scale disturbances such as Moreton waves, type II, and III radio bursts were observed, which we suggest as evidence for the blow-out of the envelope field and particle acceleration. Finally the flare arcade formed along the neutral line as the opened legs of the envelop field reconnect with each other. This dataset therefore supports the idea that the eruption may start in the sheared core field and proceeds outward with the rising plasmoid via the runaway tether-cutting reconnection and finally becomes a CME.This work is supported by NSF/SHINE grant ATM-0548952, NSF grant ATM-0536921, and NASA grant NNG0-4GJ51G.

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