SUNSPOT ROTATION, FLARE ENERGETICS, AND FLUX ROPE HELICITY: THE ERUPTIVE FLARE ON 2005 MAY 13
- Montana State University, Bozeman, MT 59715 (United States)
We use the Michelson Doppler Imager 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{sup 0} rotation of its leading polarity sunspot over 40 hr. We describe a method for including such rotation in the framework of the Minimum Current Corona 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 x 10{sup 31} erg) and flux rope self-helicity (-7.1 x 10{sup 42} Mx{sup 2}). This makes the results consistent with observations: the energy derived from GOES is 1.0 x 10{sup 31} erg, the magnetic cloud helicity from WIND is -5 x 10{sup 42} Mx{sup 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.
- OSTI ID:
- 21367368
- Journal Information:
- Astrophysical Journal, Vol. 704, Issue 2; Other Information: DOI: 10.1088/0004-637X/704/2/1146; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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