محسن جواهریان

Here, we analyzed magnetic elements of the solar active regions (ARs) observed in the line-of-sight magnetograms (the 6173 Å Fe I line) recorded with the Solar Dynamics Observatory (SDO) / Helioseismic and Magnetic Imager (HMI). The Yet Another Feature Tracking Algorithm (YAFTA) was employed to analyze the statistical properties of these features (e.g., filling factor, magnetic flux, and lifetime). Magnetic features were extracted from the areas of 180′′ × 180′′ inside the flaring AR (NOAA 12443) for 3 to 5 November 2015 and nonflaring AR (NOAA 12446) for 4 to 6 November 2015. The mean filling factor of polarities was obtained to be about 0.49 for the flaring AR; this value was 0.08 for the non-flaring AR. Time series of the filling factors of the negative and positive polarities for the flaring AR showed anti-correlated behavior (with the Pearson value of -0.80); however, for the non-flaring AR, there was a strong positive correlation (with the Pearson value of 0.95). A power-law function was fitted to the frequency distributions of flux (F), size (S), and lifetime (T). Power exponents of the distributions of flux, size, and lifetime for the flaring AR were obtained to be -2.36±0.27, -3.11±0.17, and -1.70±0.29, respectively; these values of exponents for the non-flaring AR were found to be -2.53±0.20, -3.42±0.21, and -1.61±0.19, respectively. The code detected a magnetic element with the maximum flux of 23.54×10^{20} Mx. The maximum size of detected patches was found to be about 300 Mm^2 . The most long-lived patch in the flaring AR belonged to an element with a lifetime of 2208 minutes. It was revealed that S, F , and T for patches in the flaring AR follow empirical scaling relations as S ∝ F^{0.66±0.01}, F ∝ T^{0.48±0.04}, and S ∝ T^{0.32±0.02}, respectively; For appeared patches in the non-flaring AR, these relations were obtained as S ∝ F^{0.64±0.02}, F ∝ T^{0.37±0.06}, and S ∝ T^{0.23±0.03}, respectively. The comparisons indicated that values of correlations b