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

• Autorzy: Moradhaseli M. A. , Javaherian M. , Fathalian N. , Safari H.

Identyfikatory

DOI

10.32023/0001-5237/71.2.5

• Języki publikacji: EN

Abstrakty

EN

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 180^o×180^o 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∼F^0.66±0.01, F∼T^0.48±0.04, and S∼T^0.32±0.02, respectively. For patches in the non-flaring 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 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.

Słowa kluczowe

EN

Sun: flares; Sun: photosphere; Sun: magnetic fields; methods: data analysis; methods: statistical

• Wydawca: Copernicus Foundation for Polish Astronomy
• Czasopismo: Acta Astronomica
• Rocznik: 2021
• Tom: Vol. 71, No. 2
• Strony: 163--188
• Opis fizyczny: Bibliogr. 50 poz., rys., tab., wykr.

Twórcy

autor

Moradhaseli M. A.

• Department of Physics, Faculty of Science, University of Zanjan, 45195-313, Zanjan, Iran

autor

Javaherian M.

• Research Institute for Astronomy and Astrophysics of Maragha (RIAAM), University of Maragheh, 55136-553, Maragheh, Iran

autor

Fathalian N.

• Department of Physics, Payame Noor University (PNU), 19395-3697, Tehran, Iran

autor

Safari H.

• Department of Physics, Faculty of Science, University of Zanjan, 45195-313, Zanjan, Iran

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Uwagi

Opracowanie rekordu ze środków MEiN, umowa nr SONP/SP/546092/2022 w ramach programu "Społeczna odpowiedzialność nauki" - moduł: Popularyzacja nauki i promocja sportu (2022-2023)