Empirical Scaling Relations for the Photospheric Magnetic Elements of the Flaring and NonFlaring Active Regions
Abstract
Here, we analyze magnetic elements of the solar active regions (ARs) observed in the lineofsight magnetograms (the 6173 Å FeI 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^{o}×180^{o} inside the flaring AR (NOAA 12443) for November 35, 2015 and nonflaring AR (NOAA 12446) for November 46, 2015. The mean filling factor of polarities was found to be about 0.49 for the flaring AR, while this value was 0.08 for the nonflaring AR. Time series of the filling factors of the negative and positive polarities for the flaring AR showed anticorrelated behavior (with the Pearson value of 0.80). However, there was a strong positive correlation (with the Pearson value of 0.95) for the nonflaring AR. A powerlaw 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 found to be 2.36±0.27, 3.11±0.17, and 1.70±0.29, respectively, while for the nonflaring AR: 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 longlived patch in the flaring AR belonged to an element with a lifetime of 2208 min. We showed that S, F, and T for patches in the flaring AR follow empirical scaling relations: S∼F^{0.66±0.01}, F∼T^{0.48±0.04}, and S∼T^{0.32±0.02}, respectively. For patches in the nonflaring AR, we obtained S∼F^{0.64±0.02}, F∼T^{0.37±0.06}, and S∼T^{0.23±0.03}, respectively. The comparisons indicated that correlations between parameters of F and T, and also, S and T for the flaring AR, are larger than those of the nonflaring AR. The scaling law relation between the flux growth rate of positive polarities and their size indicates a strong correlation of more than 0.7 in both ARs.
 Publication:

Acta Astronomica
 Pub Date:
 June 2021
 DOI:
 10.32023/00015237/71.2.5
 arXiv:
 arXiv:2109.12924
 Bibcode:
 2021AcA....71..163M
 Keywords:

 Sun: flares;
 Sun: photosphere;
 Sun: magnetic fields;
 Methods: data analysis;
 Methods: statistical;
 Astrophysics  Solar and Stellar Astrophysics
 EPrint:
 25 pages, 11 figures