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

Moradhaseli M. A., Javaherian M., Fathalian N., Safari H.

Acta Astronomica

2021

Vol. 71, No. 2

163--188

Here, we analyze magnetic elements of the solar active regions (ARs) observed in the line-of-sight magnetograms (the 6173 Å FeI line) recorded with the Solar Dynamics Observatory (SDO)/Hel\-ioseismic 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 180o×180o inside the flaring AR (NOAA 12443) for November 3-5, 2015 and non-flaring AR (NOAA 12446) for November 4-6, 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 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, there was a strong positive correlation (with the Pearson value of 0.95) for the non-flaring AR. 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 found to be -2.36±0.27, -3.11±0.17, and -1.70±0.29, respectively, while for the non-flaring 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 23.54×1020 Mx. The maximum size of detected patches was found to be about 300 Mm2. The most long-lived 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∼F0.66±0.01, F∼T0.48±0.04, and S∼T0.32±0.02, respectively. For patches in the non-flaring AR, we obtained S∼F0.64±0.02, F∼T0.37±0.06, and S∼T0.23±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 non-flaring 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.

Dynamical Evolution of Magnetic Flux Tube in the Solar Convective Zone

Samujłło M.

Acta Astronomica

1998

Vol. 48, No. 4

789--802

We present computations of nonlinear development of the kink instability in a horizontal magnetic flux tube lying initially in the deep convective zone. Obtained results are compared with an independent solution of the problem obtained formerly by Moreno-Insertis (1986). Consistency of solutions allows to evaluate the numerical code, in particular the treatment of the energy balance which is different than that of Moreno-Insertis.