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Sunspot Rotation, Flare Energetics and Flux Rope Helicity: The Eruptive Flare on 2005 May 13 View all abstracts by submitter

Maria D Kazachenko   Submitted: 2009-09-15 22:42

We use MDI and TRACE observations of photospheric magnetic and velocity fields in NOAA 10759 to build a three-dimensional coronal magnetic field model. The most dramatic feature of this active region is the 34 degree rotation of its leading polarity sunspot over 40 hours. We describe a method for including such rotation in the framework of the minimum current corona (MCC) model. We apply this method to the buildup of energy and helicity associated with the eruptive flare of 2005 May 13. We find that including the sunspot rotation almost triples the modeled flare energy (1.0 imes1031ergs) and flux rope self helicity (-7.1 imes1042, { m Mx}^2). This makes the results consistent with observations: the energy derived from GOES is 1.0 imes1031ergs, the magnetic cloud helicity from WIND is -5 imes1042, { m Mx}^2. Our combined analysis yields the first quantitative picture of the helicity and energy content processed through a flare in an active region with an obviously rotating sunspot and shows that rotation dominates the energy and helicity budget of this event.

Authors: Maria D. Kazachenko, Richard C. Canfield, Dana W. Longcope, Jiong Qiu, Angela DesJardins, Richard W. Nightingale
Projects: SoHO-MDI,TRACE

Publication Status: accepted for publication in ApJ
Last Modified: 2009-09-16 08:00
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