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《中国天文和天体物理学报(英文版)》 1986-01
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X-Ray,H_α,and Radio Observational Study of the 4N/X2.3 Flare of April 1,1981

Wang Jialong Han Chuanshou Xuan Jiayu Li Suchuan Zhao Eenyang Beijing Observatory, Academia SinicaDepartment of Astronomy, Nanjing UniversityYunnan Observatory, Academia Sinica  
A number of major flares were observed and studied since 19th solar cycle, but important questions such as the relation between sources in different wave ranges are still open, A combined study of space and ground-based observations in various wave ranges of a big burst might produce some useful results for resolving these problems. The 4N/X2.3 flare of April 1, 1981, one of the most intense events occurring during the cycle 21, is investigated in this paper by means of the relevant Hα, white light. X-ray (Hinotori satellite) data and radio data mainly supplied by Culgoord and Learm-onth Observatories.The disappearence or contraction of the bright bridges in Sunspots A and C, the growth of Sunspot F, and in particular, the movement of minor Sunspots E1 and E2 (see Figs. 2, 3) might be the direct cause of the occurence of the great flare studied. The disappearence of bright bridges might be one kind of EMF.The consistence of peaks in X-ray and microwave emission (Fig. 6), the relation between 35 GHz and X-ray sources as pointed by Kawabata et al. (1982), and the work by Takakura et al. (1984) show observational evidence for that the soft and hard X-ray emission and microwave emission have a common source of the event.A superimposed map of the hard X-ray (13-29 keV) source. Hα ribbon, and potential field (Fig. 9) shows that the main part of the hard X-ray source locates at the ridge of the close magnetic arcade above the north-west part of the Hα flare, and has a height of 2×10 km above the photosphere.Taking the flux of the first peak (0136 UT) in microwave as 2000 sfu and the width of the pulse as 3 minutes, the energy supplied by non-thermal electrons with energy≥20 keV during the first peak is estimated as 4.3×1031 ergs according to the figure given by Hudson et al. (1978) for a thick target.The authors are deeply indebted to Dr. G. J, Nelson at Culgoora Observatory for valuable help and supplying data, and thank the staff of Learmonth Observatory for relevant data.
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【References】
Chinese Journal Full-text Database 1 Hits
1 Xuan Jiayu, Li Suchuan, Luan Di;The Optical Omen And Active Feature of the 4N-Flare Loops on the Solar Surface on April 1,1981[J];;1986-01
【Co-citations】
Chinese Journal Full-text Database 3 Hits
1 Gui-Ping Wu, Guang-Li Huang and Yu-Hua TangDepartment of Physics, Southeast University, Nanjing 210096; Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008Department of Astronomy, Nanjing University, Nanjing 210093;The Influence of Ion-Acoustic Turbulence on the Electron Acceleration in the Reconnecting Current Sheet[J];中国天文和天体物理学报(英文版);2005-01
2 WU Gui Ping 1 XU Ao Ao 2 TANG Yu Hua 2 (1 Faculty of Physics, Nanjing Railway Medical College, Nanjing 210009) (2 Department of Astronomy, Nanjing University, Nanjing 210093);EVOLUTIONARY CHARACTERISTICS OF THE ENERGETIC ELECTRONS ACCELERATED BY ELECTRIC FIELDS IN THE PROCESS OF MAGNETIC RECONNECTION IN SOLAR ACTIVE REGIONS[J];ACTA ASTRONOMICA SINICA;2000-04
3 Xuan Jiayu, Li Suchuan, Luan Di;The Optical Omen And Active Feature of the 4N-Flare Loops on the Solar Surface on April 1,1981[J];;1986-01
【Co-references】
Chinese Journal Full-text Database 2 Hits
1 Tang Yu-hua Xu Ao-ao(Nanjing University);THE FLARE ON THE SOLAR DISK ON JULY 14,1980 AND EMF FLARE MODEL[J];Chinese Journal of Space Science;1983-04
2 Luo BAO-RONG(Yunnan Observatory, Academia Sinica);THE FLARES OF SPOTLESS REGIONS[J];Acta Astronomica Sinica;1982-02
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