太阳风速度及日球电流片对CME渡越时间的影响

罗天; 解妍琼

doi:10.11728/cjss2013.04.381

太阳风速度及日球电流片对CME渡越时间的影响

doi: 10.11728/cjss2013.04.381

罗天^1,2,
解妍琼³

1.
中国科学院空间科学与应用研究中心空间天气学国家重点实验室北京 100190
2.
中国科学院大学北京 100049
3.
解放军理工大学气象海洋学院南京 211101

基金项目: 国家自然科学基金项目资助(41231068)

详细信息

作者简介:
解妍琼, yqxie@spaceweather.ac.cn

中图分类号: P353
计量
- 文章访问数: 2378
- HTML全文浏览量: 27
- PDF下载量: 1061
- 被引次数: 0
出版历程
- 收稿日期: 2012-04-18
- 修回日期: 2013-05-25
- 刊出日期: 2013-07-15

Influence of Solar Wind Speed and Heliospheric Current Sheet on the CMEs Transit Time

LUO Tian^1,2,
XIE Yanqiong³

1.
State Key Laboratory of Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100190
2.
University of Chinese Academy of Sciences, Beijing 100049
3.
College of Meteorology and Oceanography, PLA University of Science and Technology, Nanjing 211101

摘要

摘要: 基于1996-2005年88个引起重大地磁暴的CME(日冕物质抛射)事件、1996-2000年的47个CME事件以及1997-2002年的29个全晕状CME事件,结合ACE卫星在1AU处的太阳风和行星际磁场观测资料以及Wilcox Solar Observatory(WSO)天文台的太阳光球层磁图,分析了背景太阳风速度和日球电流片对CME到达1AU处渡越时间预报误差的影响.结果表明,背景太阳风速度与CME渡越时间误差并没有明显的相关性,在考虑了磁云通量管轴相对黄道面夹角的影响后相关性依然不明显.然而日球电流片对CME渡越时间却有明显的影响,对于初速度较小的异侧CME事件,其渡越时间大于同侧事件;而对于具有较大初速度的CME事件,异侧事件的渡越时间明显小于同侧事件.研究结果表明,CME与太阳风以及日球电流片的相互作用并不是简单的对流相互作用,造成高速CME异侧事件快于同侧事件到达地球的因素非常复杂,有待深入研究.
- CME渡越时间 /
- 背景太阳风速度 /
- 日球电流片
Abstract: 88 CME events that cause significant geomagnetic storms, 47 CME events and 27 Full Halo CME events, along with the ACE spacecraft observations of interplanetary solar wind and ICME at 1AU, as well as the magnetic graph on the solar photosphere assembled by Wilcox Solar Observatory (WSO), are used to analyze the effect of various conditions of both ambient solar wind speed and heliospheric current sheet on the CME transit time to the Earth. The results demonstrate that the ambient solar wind speed and the CME transit time errors show little correlation, even after taking into account of the effect of the angle between magnetic cloud flux tube and the ecliptic plane. However, the heliospheric current sheet exerts significant influences on the CME transit time. For CMEs with relatively lower initial velocity, the transit time of the opposite side events is longer than that of the same side events (if the earth and the source of CME are on the opposite side of the current sheet it is called a opposite side event, otherwise it is called a same side event). For CMEs with higher initial velocity, the transit time of the opposite side events is shorter than that of the same side events. The result is contrary to our expectations that the current sheet will impede the dissemination of ICMEs in the interplanetary space and thus extend the transit time. One possible explanation is that the interaction of CMEs with solar wind and the current sheet is not simply the convective interaction and the mechanism behind this phenomenon is very complex and requires further study.
- CME transit time /
- Ambient solar wind speed /
- Heliospheric current sheet

HTML全文

参考文献(18)

[1]	Feng Xueshang, Xiang Changqing, Zhong Dingkun. The state-of-art of three-dimensional numerical study for corona-interplanetary process of solar storms[J]. Sci. Sin. Terr., 2011, 41(1):1-28
[2]	Gopalswamy N, Lara A, Lepping R P. Interplanetary acceleration of coronal mass Ejections[J]. Geophys. Res. Lett., 2000, 27(2):145-148
[3]	Gopalswamy N, Lara A, Yashiro S, et al. m Predicting the 1-AU arrival times of coronal mass ejections[J], J. Geophys. Res., 2001, 106(A12):29207-29217
[4]	Manoharan P K, Gopalswamy N, Yashiro S, et al. m Influence of coronal mass ejection interaction on propagation of interplanetary shocks[J]. J. Geophys. Res., 2004, 109, A06109, DOI: 10.1029/2003JA010300
[5]	Schwenn R, Dal Lago A, Huttunen E, Gonzalez W D. The association of coronal mass ejections with their effects near the Earth[J]. Ann. Geophys., 2005, 23(3):1033-1059
[6]	Srivastava N, Venkatakrishnan P. Solar and interplanetary sources of major geomagnetic storms during 1996-2002[J]. J. Geophys. Res., 2004, 109, A10103, DOI: 10.1029/2003JA010175
[7]	Vrsnak B, Gopalswamy N. Influence of aerodynamic drag on the motion of interplanetary ejecta[J]. J. Geophys. Res., 2002, 107(A2), 1019, DOI: 10.1029/2001JA000120
[8]	Wang Y M, Ye P Z, Wang S, Zhou G P, Wang J X. A statistical study on the geoeffectiveness of Earth-directed coronal mass ejections from March 1997 to December 2000[J]. J. Geophys. Res., 2002, 107(A11), 1340, DOI: 10.1029/2002JA009244
[9]	Zhang J, Dere K P, Howard R A, Bothmer V. Identification of solar sources of major geomagnetic storms between 1996 and 2000[J]. Astrophys. J., 2003, 582:520-533
[10]	Zhao Xinhua. Statistical Analysis on the Solar-terrestrial Transients and Comprehensive Research on the Related Prediction Methods[D]. Beijing: Graduate University of Chinese Academy of Sciences, 2007
[11]	Wei F S, Feng X S, Xu Y, Fan Q L. Prediction tests by using "ISF" method for the geomagnetic disturbances[J]. Adv. Space Res., 2005, 36(12):2363-2367
[12]	Xie Y Q, Wei F S, Feng X S, Zhong D K. Prediction test for the two extremely strong solar storms in October 2003[J]. Solar Phys., 2006, 234(2):363-377
[13]	Wei F S, Dryer M. Propagation of solar flare-associated interplanetary shock waves in the heliospheric meridional plane[J]. Solar Phys., 1991, 132:373-394
[14]	Xie Y Q, Wei F S, Xiang C Q, Feng X S. The effect of heliospheric current sheet on interplanetary shocks[J]. Solar Phys., 2006, 238(2):377-390
[15]	Feng X S, Zhao X H. Geoeffective analysis of CMEs under current sheet magnetic coordinates[J]. Astrophys. Space Sci., 2006, 305(1):37-47
[16]	Zhang J, Richardson I G, Webb D F, et al. m Solar and interplanetary sources of major geomagnetic storms (Dst<-100nT) during 1996-2005[J]. J. Geophys. Res., 2007, 112, A10102, doi: 10.1029/2007JA012321
[17]	Gopalswamy N, Lara A, Manoharan P K, Howard R A. An empirical model to predict the 1-AU arrival of interplanetary shocks[J]. Adv. Space Res., 2005, 36:2289-2294
[18]	Burlaga L, Sittler E, Mariani F, Schwenn R. Magnetic loop behind an interplanetary shock: Voyager, Helios, and IMP 8 observations[J]. J. Geophys. Res., 1981, 86(A8):6673-6684