多方向<i>μ</i>介子通量一致性特征研究

薛炳森; 苍中亚; 张吉龙

doi:10.11728/cjss2017.06.667

多方向μ介子通量一致性特征研究

doi: 10.11728/cjss2017.06.667

1. 中国气象局空间天气重点开放实验室北京 100081;
2. 南京信息工程大学空间天气研究所南京 210044;
3. 中国科学院高能物理研究所北京 100049

基金项目:

国家自然科学基金项目资助（11575204）

详细信息

作者简介:
薛炳森,xuebs@cma.gov.cn

中图分类号: P352
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出版历程
- 收稿日期: 2016-11-21
- 修回日期: 2017-05-08
- 刊出日期: 2017-11-15

Study of Multi-directional muon flux in geomagnetic storm prediction

1. Key Laboratory of Space Weather, China Meteorological Administration, Beijing 100081;
2. Institute of Space Weather, Nanjing University of Information Science and Technology, Nanjing 210044;
3. Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049

摘要

摘要: 通过地面μ介子望远镜可以探测不同方向到达的宇宙线通量，得到从外空间入射的宇宙线受到不均匀结构的调制情况，判断CME的特征.通过分析，发现大地磁暴前Nagoya台站东向和南向的探测数据存在固定的2h时间差，认为这是由两个入射方向的宇宙线粒子先后穿越CME结构引起的.分别计算了两个方向相同时间和南向相位后移2h后通量探测数据的相关系数，以及两种情形下通量差的变化幅度，定量描述了CME接近地球过程中两个方向通量的相关特征.通过比较发现，CME接近地球过程中，经过相位变换的两个方向的相关系数明显高于未经变换的情况，经过相位变换的两个方向的通量差幅度明显小于未经变换的情况；CME到达地球后，两种情形的相关系数和通量差幅度则趋于相同.对2003-2005年K_p=9的地磁暴事件的分析均发现了这种现象.对2006年12月14日大地磁暴前的μ介子通量特征进行了分析，也完全符合上述特征.
- μ介子 /
- 多方向 /
- 相关分析 /
- 地磁暴
Abstract: By analyzing the characteristics of cosmic ray flux evolution, the approaching of CMEs could be identified, and the geomagnetic disturbance could be forecasted. The modulation of cosmic by CMEs could be derived by comparing the fluxes from different directions, and the parameters, such as Interplanetary Magnetic Field (IMF) and direction, could be derived. In this paper, data obtained by Nagoya muon telescope are used, and southward and eastward flux are chosen for investigation in detail. The results show that the evolutions of muon fluxes from the two directions share similar pattern before the strong geomagnetic storm, while there is a 2-hour phase delay between them. It is analyzed that the cosmic rays corresponding to the two directions went into and out the CME successively and the time difference is about 2 hours. The correlation coefficient and flux difference of the fluxes in eastern and southern, concluding the phase of the southern flux is moved backward two hours or not, are calculated respectively. As CMEs approaching, the correlation coefficient with southward phase change is significantly higher than that without phase change, and the flux difference with the southward phase change is much lower than that without phase change. However, the coefficient and the flux difference began to get close to each other when CMEs arrive at the Earth. And the above parameters of phase changed disparity amplitude even exceeded the unchanged one. The characteristics are also found in the geomagnetic storms with K_p=9 from 2003 to 2005. The muon flux before the great geomagnetic storm on December 14, 2006 is analyzed, and the study found that it is coincident with the above characteristics. Therefore, directional muon detection possesses a unique ability to remote sensing CMEs propagation through the difference of the flux evolution from different directions.
- Muon /
- Multi-direction /
- Correlation analysis /
- Geomagnetic storms

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参考文献(14)

[1]	JOSELYN J A. Geomagnetic activity forecasting:the sta-te of the art[J]. Rev. Geophys., 1995, 33(3):383-401
[2]	KUDELA K, STORINI M, HOFER M, et al. Cosmic rays in relation to space weather[J]. Space Sci. Rev., 2000, 93(1/2):153-174
[3]	RUFFOLO D. Transport and acceleration of energetic charged particles near an oblique shock[J]. Astrophys. J., 1999, 515(2):787-800
[4]	DORMAN L I, IUCCI N, VILLORESI G. The use of cosmic rays for continuous monitoring and prediction of some dangerous phenomena for the earth's civilization[J]. Astrophys. Space Sci., 1993, 208(1):55-68
[5]	DORMAN L I, IUCCI N, VILLORESI G. Possible monitoring of space processes by cosmic rays[C]//Proceedings of the 23rd International Cosmic Ray Conference. Alberta, Canada:University of Calgary, 1993:695-698
[6]	DORMAN L I, IUCCI N, VILLORESI V. The nature of cosmic ray Forbush-decrease and precursory effec-ts[C]//Proceedings of the 24th International Cosmic Ray Conference. Rome, Italy:International Union of Pure and Applied Physics, 1995:892-895
[7]	DORMAN L I, PUSTIL'NIK L A, STERNLIEB A, et al. Monitoring and forecasting of great solar proton events using the neutron monitor network in real time[J]. IEEE Trans. Plasma Sci., 2004, 32(4):1478-1488
[8]	SAVIAN J F, DA SILVA M R, VIEIRA L E A, et al. Forbush decreases for 2001-2004 observed with low la-titude muon telescopes of Brazilian SSO observatory[J]. Geophys. Res. Abstr., 2005, 7:340
[9]	MUNAKATA K, BIEBER J W, YASUE S I, et al. Precursors of geomagnetic storms observed by the muon detector network[J]. J. Geophys. Res., 2000, 105(A12):27457-27468
[10]	LE Guiming, YE Zonghai, YU Shaohua, et al. Wavelet analysis of the cosmic ray intensities at Guangzhou muon station during January 7-11, 1997[J]. Chin. J. Geophys., 2004, 47(2):190-194
[11]	WANG Jing, LIU Siqing, XUE Bingsen, et al. Anisotropy analyses of cosmic ray before the geomagnetic storm on Sept. 24, 1998[J]. Chin. J. Space Sci., 2009, 29(5):495-501
[12]	KANE R P. Directional muon telescopes not useful for estimating the magnitudes of Forbush decreases and geo-magnetic storms[J]. Indian J. Radio Space Phys., 2011, 40:76-84
[13]	SABBAH I, TOKUMARU S M, DULDIG M L, et al. First observed coronal mass ejection from the middle east using cosmic rays[J]. Kuwait J. Sci. Eng., 2010, 37(2):43-61
[14]	DE MENDONCA R R S, RAULIN J P, ECHER E, et al. Analysis of atmospheric pressure and temperature effects on cosmic ray measurements[J]. J. Geophys. Res.:Space Phys., 2013, 118(4):1403-1409