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The magnetic non-potentiality is important for understanding flares and othersolar activities in active regions (ARs). Five non-potential parameters, i.e.,electric current, current helicity, source field, photospheric free energy, andangular shear, are calculated in this work to quantify the non-potentiality ofNOAA AR 11158. Benefited from high spatial resolution, high cadence, andcontinuously temporal coverage of vector magnetograms from the Helioseismic andMagnetic Imager on board the Solar Dynamics Observatory, both the long-termevolution of the AR and the rapid change during flares have been studied. Weconfirmed that, comparing with the magnetic flux, the magnetic non-potentialityhas a closer connection with the flare, and the emerging flux regions areimportant for the magnetic non-potentiality and flares. The main results ofthis work are as follows. (1) The vortex in the source field directly displaysthe deflection of horizontal magnetic field. The deflection is corresponding tothe fast rotated sunspot with a time delay, which suggests that the sunspotrotation leads to an increase of the non-potentiality. (2) Two areas that haveevident changes of the azimuth of the vector magnetic field are found near themagnetic polarity inversion line. The change rates of the azimuth are about 1.3deg/h and 3.6 deg/h, respectively. (3) Rapid and prominent increases are foundin the variation of helicity during four flares in their initial brighteningregions. The recovery of the increases takes 3-4 h for the two biggest flares(X2.2 and M6.6), while only takes about 2 h for the other two smaller flares(M2.2 and M1.6).

Flares and Magnetic Non-potentiality of NOAA AR 11158