The curious temporal behavior of the frequency of different class flares |
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| Institution: | 1. Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China;2. Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;3. Kunming No.3 Middle School, Kunming 650011, China;1. NASRDA-Centre for Basic Space Science, Nsukka, Enugu State, Nigeria 410001, Nsukka, Nigeria;2. Department of Physics and Astronomy, University of Nigeria, Nsukka, Enugu State, Nigeria 410001, Nsukka, Nigeria;1. Division of Theoretical Astronomy, National Astronomical Observatory of Japan,2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan;2. Department of Natural Science, Kochi University, 2-5-1 Akebono-cho, Kochi 780-8520, Japan;3. Department of Human Informatics, Aichi Shukutoku University, 2-9 Katahira, Nagakute, Aichi 480-1197, Japan;1. Theory Group, Department of Physics and Texas Cosmology Center, The University of Texas at Austin, TX 78712, USA;2. Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA;1. Physics Department, University of Rijeka, Radmile Matej?i?, 51000 Rijeka, Croatia;2. INAF Astronomical Observatory of Padova, via dell’Osservatorio 8, Asiago (VI) 36012, Italy;1. Sarojini Naidu College for Women, Kolkata 700028, India;2. Camellia Institute of Engineering, Kolkata 700129, India;3. St. Xavier’s College (Autonomous), Kolkata 700016, India;4. Harish Chandra Research Institute, Allahabad 211019, India |
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| Abstract: | We investigate the frequency of all (X-ray flare events higher than class B1.0), B, C, M and X-class flares, respectively, derived from the National Geophysical Data Center (NGDC) list of solar flares between May 1983 and September 2014, which corresponds to the two complete solar cycles (SCs) 22 and 23 as well as the rise and maximum phases of SC 24. Analysis shows that the temporal behavior for these various class flares is quite different. The main findings of this study, confirmed by using the Hinode flare catalog where possible, are as follows. (1) The B-class flares are in complete antiphase with all, C, M and X-class flares. (2) While, there is a small decreasing trend in the peak values of the smoothed monthly C-class flare numbers from SC 22 to 24, the occurrence rate of M and X-class flares dropped by almost half and two-thirds, respectively, during SC 23 and remained almost the same during SC 24. This class-dependent temporal behavior provides support for dynamo models that involve the coexistence of a deep global and a superficial local dynamo. |
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