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Here, we analyzed magnetic elements of the solar active regions (ARs)observed in the line-of-sight magnetograms (the 6173 \AA~Fe \small{I} line)recorded with the Solar Dynamics Observatory (SDO)/Helioseismic and MagneticImager (HMI). The Yet Another Feature Tracking Algorithm (\textsf{YAFTA}) wasemployed to extract the statistical properties of these features (\textit{e.g.}filling factor, magnetic flux, and lifetime) within the areas of$180{\small^{\prime\prime}} \times 180{\small^{\prime\prime}}$ inside theflaring AR (NOAA 12443) and the non-flaring AR (NOAA 12446) for 3 to 5 November2015 and for 4 to 6 November 2015, respectively. The mean filling factor ofpolarities was obtained to be about 0.49 for the flaring AR; this value was0.08 for the non-flaring AR. Time series of the filling factors of the negativeand positive polarities for the flaring AR showed anti-correlation (with thePearson value of -0.80); while for the non-flaring AR, there was the strongpositive correlation (with the Pearson value of 0.95). A power-law function wasfitted to the frequency distributions of flux ($F$), size ($S$), and lifetime($T$). Power exponents of the distributions of flux, size, and lifetime for theflaring AR were obtained to be about -2.36, -3.11, and -1.70, respectively;these values of exponents for the non-flaring AR were found to be about -2.53,-3.42, and -1.61, respectively. ...

Empirical Scaling Relations for the Photospheric Magnetic Elements of the Flaring and Non-Flaring Active Regions