第23至24周太阳质子事件的统计特征

白铁男; 乐贵明; 赵浩峰

doi:10.11728/cjss2017.06.649

第23至24周太阳质子事件的统计特征

doi: 10.11728/cjss2017.06.649

白铁男^1,2,3,
乐贵明^2,3,
赵浩峰¹

1. 南京信息工程大学数学与统计学院南京 210044;
2. 中国气象局空间天气重点开放实验室北京 100081;
3. 国家空间天气监测预警中心北京 100081

基金项目:

国家自然科学基金项目（41074132，41274193，41474166）和质检总局行业专项（200710123）共同资助

详细信息

作者简介:
乐贵明,legm@cma.gov.cn

中图分类号: P353
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出版历程
- 收稿日期: 2016-12-07
- 修回日期: 2017-05-21
- 刊出日期: 2017-11-15

Statistical Properties of Solar Proton Events during Solar Cycle 23 and 24

1. Department of Physics and Optoelectronic Technology, Nanjing University of InformationScience and Technology, Nanjing 210044;
2. Key Laboratory of Space Weather, China Meteorological Administration, Beijing 100081;
3. National Center for Space Weather, Beijing 100081

摘要

摘要: 第23至24太阳活动周（1997-2016年）期间太阳质子事件的强度统计分析表明，1997-2016年期间总共发生了128个太阳质子事件，其中峰值通量范围为10~99pfu，100~999pfu，1000~2999pfu及>3000pfu的事件分别占55.15%，27.94%，9.56%，7.35%.太阳质子事件的不对称性分析表明，不同强度太阳质子事件东西不对称性的程度不相同，其中1000~2999pfu事件的不对称性最强，而3000pfu以上事件的不对称性最弱.第23周期间，太阳质子事件主要发生在太阳活动周两个峰值之间和最大峰值之后的时段，而第24周太阳质子事件主要发生在太阳活动周最大峰值之前.
- 太阳黑子 /
- 质子事件 /
- 不对称性 /
- 太阳活动周
Abstract: There were totally 128 Solar Proton Events (SPEs) from 1997 to 2016. Their peak flux ranges are from 10pfu to 99pfu, 100 to 999pfu, 1000 to 2999pfu and greater than 3000pfu, and the percentage is 55.15%, 27.94%, 9.56% and 7.35% respectively. The results show that SPEs with different peak flux have different asymmetry. The SPEs with peak flux ranged from 1000pfu to 2999pfu have the largest asymmetry, while those with peak flux greater than 3000pfu have smallest asymmetry. In Solar Cycle 23, the SPEs mainly occurred during the period from the first peak to the second peak and after the second peak of the smoothed monthly mean sunspot numbers. In Solar Cycle 24, the SPEs mainly occurred during the period before maximum of smoothed monthly mean sunspot numbers.
- Sunspots /
- Proton events /
- Asymmetry /
- Solar activity cycle

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参考文献(18)

[1]	REAMES D V. Particle acceleration at the Sun and in the heliosphere[J]. Rev. Space Sci., 1999, 90(3/4):413-419
[2]	TYLKA A J, COHEN C M S, DIETRICH W F, et al. Shock geometry, seed populations, and the origin of variable elemental composition at high energies in large gra-dual solar particle events[J]. Astrophys. J., 2005, 625(1):474-495
[3]	GOPALSWAMY N, YASHIRO S, MICHALEK G, et al. Interacting coronal mass ejections and solar energetic particles[J]. Astrophys. J., 2002, 572(1):L103-L107
[4]	RICHARDSON I G, LAWRENCE G R, HAGGERTY D K, et al. Are CME interactions really important for accele-rating major solar energetic particle events[J]. Geophys. Res. Lett., 2003, 30(12):8014
[5]	KAHLER S W, VOURLIDAS A. Do Interacting coronal mass ejections play a role in solar energetic particle events[J]. Astrophys. J., 2014, 784(1):47
[6]	CHEN Minhao, CHEN Yulin, LE Guiming, et al. Dependence of the intensity of solar energetic particle event on the twin-CME:two cases study[J]. Chin. J. Space Sci., 2016, 36(3):267-271(陈#
[7]	CANE H V, RICHARDSON I G, VONROSENVINGE T T. A study of solar energetic particle events of 1997-2006:their composition and associations[J]. J. Geophys. Res., 2010, 115(A8):A08101
[8]	KUBO Y, AKIOKA M. Existence of thresholds in proton flares and application to solar energetic particle alerts[J]. Space Weather, 2004, 2(1):S01002
[9]	LE Guiming. The Carrington longitude distribution of solar proton event source locations during 1997-2003[J]. Chin. J. Space Sci., 2004, 24(2):81-88(乐贵明. 1997-2003年太阳质子事件源区的卡林顿经度分布[J]. 空间科学学报, 2004, 24(2):81-88)
[10]	昊, 陈玉林, 乐贵明, 等. 太阳高能粒子事件强度与相关双CME事件关系的两个事例[J]. 空间科学学报, 2016, 36(3):267-271)
[10]	LE Guiming, CHEN Yanhong. The statistical analy-sis of solar flares during the interval 1996-2002[J]. Chin. J. Space Sci., 2003, 23(5):321-328(乐贵明, 陈艳红. 1996-2002年太阳耀斑的统计分析[J]. 空间科学学报, 2003, 23(5):321-328)
[11]	CHENG Libin, LE Guiming, LU Yangping, et al. The analysis of the properties of super solar proton events and the associated phenomena[J]. Acta Astron. Sin., 2014, 55(3):203-210
[12]	MCINTOSH P S. The classification of sunspotgroups[J]. Solar Phys., 1990, 125(2):251-267
[13]	GNVEYSHEV M N. On the 11-year cycle of solar activi-ty[J]. Solar Phys., 1967, 1:107-120
[14]	GNEVYSHEV M N. Essential features of the 11-year solar cycle[J]. Solar Phys., 1977, 51(1):175-183
[15]	BAZILEVSKAYA G A, MAKHMUTOV V S, SLADKOVA A I. Gnevyshev gap effects in solar energetic particle activity[J]. Adv. Space Res., 2006, 38(3):484-488
[16]	WANG Jialong, XIAO Zuo, GAO Yufen. Study of high solar activity in February 1986 IV. A preliminary analysis of the relationship between solar and terrestrial events[J]. Chin. J. Space Sci., 1998, 18(4):290-295(王家龙, 肖佐, 高玉芬. 1986年2月的高太阳活动研究——IV日地扰动事件耦合初析[J]. 空间科学学报, 1998, 18(4):290-295)
[17]	LE Guiming, YANG Xingxing, DING Liuguan, et al. Solar cycle distribution of strong solar proton events and the related solar-terrestrial phenomena[J]. Astrophys. Space Sci., 2014, 352(2):403-408