Evolution of Magnetic Field in the Flaring Active Region AR 11158 Based on SDO/HMI Observation

Details Evolution of Magnetic Field in the Flaring Active Region AR 11158 Based on SDO/HMI Observation Evolution of Magnetic Field in the Flaring Active Region AR 11158 Based on SDO/HMI Observation

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh31a1993s&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH31A-1993

Astronomy and Astrophysics

Astrophysics

[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields

Scientific paper

We report the evolution of magnetic field and its energy in NOAA active region 11158 based on a vector magnetogram series from the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamic Observatory (SDO). Over 5 days, the quadrupolar sunspot complex produced multiple eruptions, including the first X-class flare of the current solar cycle. Extrapolated non-linear force-free coronal fields suggest substantial electric current and free energy injection during early flux emergence along a newly-formed, pronounced filament. About 75% of the inferred free energy is stored below 10 Mm; the total decreased by 0.25E32 erg (10%) within 1 hour of the X-class flare, which is likely an underestimation of the actual energy loss. During the flare, photospheric flux underwent rapid redistribution: horizontal flux density was enhanced by 28% in the AR core region. Extrapolation shows that such change is consistent with the conjectured coronal field "implosion". Multiple coronal loops retraction were indeed observed for 5 minutes over 10 Mm during the impulsive phase. Modeling indicates that the coronal field becomes more compact after the flare, its lower layers more energetic but overall less so.

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