Abstract
Precursors of the strong solar flare X1.0 (according to the Geostationary Operational Environmental Satellite (GOES) classification) recorded on March 29, 2014, in the active region (AR) 12017 are investigated. The precursors manifested themselves in the AR microwave radiation and its magnetographic characteristics. This work was carried out as part of the development of an observational database of precursors of large flares (those more powerful than class M5 according to the GOES classification) in different ARs based on an analysis of the microwave radiation and magnetographic characteristics of ARs. Further generalization and systematization of the identified precursors of strong solar flares makes it possible to move on to the development of methods for their forecasting. According to data from Solar Dynamics Observatory Helioseismic and Magnetic Imager (SDO/HMI), two days before the X flare a new magnetic flux emerged in the analyzed AR 12017 near the main spot of the group with a magnetic field sign opposite that of main spot field (formation of the δ configuration). The study of the evolution of the magnetic field gradient in the AR showed a sharp increase before the X flare, which reached its peak 8 h before the flare with a subsequent decrease before the flare. Analysis of the AR microwave radiation, which was carried out based on the results of multiwavelength multiazimuth (31 daily observations for 4 h with 8-minute intervals) spectral polarization observations of the Sun by the RATAN-600 in the range 1.65–6.0 cm for a few days before the flare, revealed the emergence and development of a microwave source over the region with the δ configuration two days before the X flare. The parameters of the radio-frequency radiation of this source make it possible to classify it as a “peculiar” microwave source that was discovered earlier by the RATAN-600 in a number of eruptive events 1–2 days before large X flares. It was found for the first time that the time variation of the intensity of the microwave source over the region with the δ configuration occurred similarly to the evolution of the magnetic field gradient in the AR.
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References
Abramov-Maximov, V.E., Borovik, V.N., Opeikina, L.V., and Tlatov, A.G., Dynamics of microwave sources associated with the neutral line and the magnetic-field parameters of sunspots as a factor in predicting large flares, Sol. Phys., 2015, vol. 290, pp. 53–77.
Akhmedov, Sh.B., Bogod, V.M., Borovik, V.N., et al., Structure of active regions on the Sun from VLA and RATAN-600 observations in July 1982, Astrofiz. Issled. (Izv. SAO), 1987, vol. 25, pp. 105–134.
Bogod, V.M., Zhekanis, G.N., Mingaliev, M.G., and Tokhchukova, S.Kh., Multi-azimuth regime of observations at the RATAN-600 southern sector with periscope reflector, Radiophys. Quantum Electron., 2004, vol. 47, no. 4, pp. 227–237.
Bogod, V.M., Alesin, A.M., and Pervakov, A.A., RATAN-600 radio telescope in the 24th solar-activity cycle. II. Multioctave spectral and polarization high-resolution solar research system, Astrophys. Bull., 2011, vol. 66, no. 2, pp. 205–214.
Cui, Y., Li, R., Zhang, L., He, Y., and Wang, H., Correlation between solar flare productivity and photospheric magnetic field properties. I. Maximum horizontal gradient, length of neutral line, number of singular points, Sol. Phys., 2006, vol. 237, pp. 45–59.
Cui, Y., Li, R., Wang, H., and He, H., Correlation between solar flare productivity and photospheric magnetic field properties II. Magnetic gradient and magnetic shear, Sol. Phys., 2007, vol. 242, pp. 1–8.
Falconer, D.A., Moore, R.L., and Gary, G.A., Correlation of the coronal mass ejection productivity of solar active regions with measures of their global nonpotentiality from vector magnetograms: Baseline results, Astrophys. J., 2002, vol. 569, pp. 63–77.
Garaimov, V.I., Processing of one-dimensional data vector arrays in Windows OS, WorkScan version 2.3, Preprint no. 127T, Nizhnii Arkhyz: SAO, 1997.
Ishkov, V.N., The emersion of magnetic flux as a key to the prediction of strong solar flares, Izv. Akad. Nauk: Ser. Fiz., 1998, vol. 62, no. 9, p. 1835–1839.
Korsos, M.B., Gyenge, N., Baranyi, T., and Ludmany, A., Dynamic precursors of flares in active region NOAA, arXiv, 2015, http://arxiv.org/abs/1501.07257.
Korsos, M.B., Baranyi, T., and Ludmany, A., Pre-flare dynamics of sunspot groups, Astrophys. J., 2014, vol. 789, id 107.
Korzhavin, A.N., Opeikina, L.V., and Peterova, N.G., Transition region above sunspots inferred from microwave observations, Astrophys. Bull., 2010, vol. 65, no. 1, pp. 63–77.
Künzel, H., Die Flare-Häfigkeit in Fleckengruppen unterschiedlicher Klasse und magnetischer Struktur, Astron. Nachr., 1960, vol. 285, pp. 271–273.
Schrijver, C.J., A characteristic magnetic field pattern associated with all major solar flares and its use in flare forecasting, Astrophys. J., 2007, vol. 655, pp. L117–L120.
Severnyi, A.B., Nekotorye problemy fiziki Solntsa (Some Problems of Solar Physics), Moscow: Nauka, 1988.
Steward, G., Lobzin, V., and Wilkinson, P.J., Automatic recognition of complex magnetic regions on the sun in gong magnetogram images and prediction of flares, in Techniques for the Flare Warning Program Flarecast, Space Weather, 2011, vol. 9, p. 11004.
Tlatov, A.G., Vasil’eva, V.V., Makarova, P.A., and Otkidychev, P.A., Applying an automatic image-processing method to synoptic observations, Sol. Phys., 2014, vol. 289, pp. 1403–1413.
Wang, H., Rapid changes of photospheric magnetic fields around flaring magnetic neutral lines, Astrophys. J., 2006, vol. 649, pp. 490–497.
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Abramov-Maximov, V.E., Borovik, V.N., Opeikina, L.V. et al. Precursors of the solar X flare on march 29, 2014, in the active region NOAA 12017 based on microwave radiation and magnetographic data. Geomagn. Aeron. 55, 1097–1103 (2015). https://doi.org/10.1134/S0016793215080022
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DOI: https://doi.org/10.1134/S0016793215080022