用三维运动学模型研究行星际激波与共转高速流的相互作用

doi:10.7523/j.issn.2095-6134.2009.2.016

中国科学院大学学报 ›› 2009, Vol. 26 ›› Issue (2): 258-267.DOI: 10.7523/j.issn.2095-6134.2009.2.016

用三维运动学模型研究行星际激波与共转高速流的相互作用

佟亚男^1,2, 刘四清¹, 刘方华¹, 龚建村¹

1. 中国科学院空间科学与应用研究中心, 北京 100190;
2. 中国科学院研究生院, 北京 100049

收稿日期:2008-03-03 修回日期:2008-10-22 发布日期:2009-03-15
通讯作者: 佟亚男
基金资助:
国家973计划(G2006CB806300)资助 

Interaction between interplanetary shock and corotating high speed stream studied by a 3-D kinematic method

TONG Ya-Nan^1,2, LIU Si-Qing¹, LIU Fang-Hua¹, GONG Jian-Cun¹

1. Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100190, China;
2. Graduate University of the Chinese Academy of Sciences, Beijing 100049, China

Received:2008-03-03 Revised:2008-10-22 Published:2009-03-15

摘要/Abstract

摘要：

利用三维运动学模型模拟研究行星际激波与共转高速流(CHSS)的相互作用。通过改变模式输入条件中耀斑的强度及位置,研究相互作用对CHSS到达地球时间的影响,以及对激波的传播和激波形态的影响。模拟结果表明:(1)行星际激波与CHSS相互作用对彼此到达地球时间都有影响;(2)有激波比没有激波条件下的CHSS到达地球时间要早,且CHSS到达地球时间与驱动激波的耀斑的强度以及扰动源区的位置有关,耀斑的强度越大、扰动源区与CHSS前的电流片的经度距离越近,则CHSS到达地球时间也越早;(3)激波在以CHSS为背景的太阳风中传播比在没有CHSS的均匀背景场中传播得快,但激波与CHSS的相互作用对激波到达地球时间的影响远没有对CHSS到达地球时间的影响大;(4)当耀斑位于CHSS前电流片的东边时,耀斑驱动的激波与CHSS相互作用可能会使激波形态发生改变,呈双峰结构。

关键词: 三维运动学模型, 行星际激波, 共转高速流

Abstract:

The interaction between interplanetary shock (IS) and corotating high speed stream (CHSS) was investigated in this paper using a 3-D kinematic method (HAF model). By changing the input conditions, such as the intensity and the location of flares, the influence of the interaction on the arrival time of CHSS was analyzed at first. Then the shock propagation effected by the interaction was studied. The simulation results showed that: (1) The interaction between IS and CHSS can influence their arrival time; (2) CHSS compressed by IS arrived earlier. Moreover, the arrival time of CHSS was associated with the intensity and location of IS's solar sources, flares. With the longitude distance between the flare and the current sheet in front of CHSS decreasing, and the flare intensity getting stronger, CHSS arrived earlier; (3) The propagation of IS under the background of CHSS was faster. But the interaction made much less influence on IS comparing with CHSS; (4) When a flare was situated at the eastern of the current sheet in front of CHSS, the shape of IS driven by the flare maybe changed and displayed two peaks structure.

Key words: 3-D kinematic model, interplanetary shock(IS), corotating high speed stream

中图分类号:

P353

佟亚男, 刘四清, 刘方华, 龚建村. 用三维运动学模型研究行星际激波与共转高速流的相互作用[J]. 中国科学院大学学报, 2009, 26(2): 258-267.

TONG Ya-Nan, LIU Si-Qing, LIU Fang-Hua, GONG Jian-Cun. Interaction between interplanetary shock and corotating high speed stream studied by a 3-D kinematic method[J]. , 2009, 26(2): 258-267.

参考文献

[1] Zhao XH. Statistical analysis on the solar-terrestrial transients and comprehensive research on the related prediction methods: . Beijing: Center for Space Science and Applied Research, Chinese Academy of Sciences, 2007 (in Chinese) 赵新华.日地扰动事件的统计分析及相关预报方法的综合研究: .北京:中国科学院空间科学与应用研究中心,2007

[2] 魏奉思.关于耀斑-激波非对称传播的统计研究.中国科学(A辑),1987, 30:186~193

[3] Wei, FS, Dryer M. Propagation of solar flare-associated interplanetary shock waves in the heliospheric meridional. Planetary Solar Physics,1991, 132:373~394

[4] Richardson IG, Cane HV, Cliver EW. Sources of geomagnetic activity during nearly three solar cycles (1972~2000). Journal of Geophysics Research, 2002, 107(A8)(doi):10.1029/2001JA000

[5] 焦维新.空间天气学.北京:气象出版社,2003

[6] Cho KS, Moon YJ, Dryer M, et al. Astatistical comparison of interplanetary shock and CME propagation models. Journal of Geophysical Research, 2003, 108(A12): 1445~1452

[7] Fry CD, Dryer M, Deehr CS, et al. Forecasting solar wind structures and shock arrival times using an ensemble of models. Journal of Geophysical Research, 2003, 108: 1070~1089

[8] Liu SQ, Wei FS. Relationship between filament disappearance events and interplanetary disturbances studied by a 3-D kinematic method. Chinese Journal of Geophysics, 1998, 41(6): 735~743(in Chinese) 刘四清,魏奉思.用三维运动学模式研究太阳暗条消失与行星际扰动.地球物理学报,1998,41(6):735~743

[9] Wang CB, Zhao JK, Chen HH, et al. Prediction of the IMF B_z using 3-D kinematic code. Chinese Journal of Geophysics, 2002, 45(6): 749~758(in Chinese) 王传兵,赵寄昆,陈合宏,等.运用三维运动学模型对行星际磁场南北分量的预测.地球物理学报,2002,45(6):749~758

[10] Liu WG. Interaction between the solar coronal mass ejections and heliospheric sector Boundary: . Taiwan: Institute of Space Science National Center University, 2004 (in Chinese) 柳文冠.日冕抛射物质对扇形边界的影响: .台湾:国立中央大学太空科学研究所,2004

[11] Xie YQ. Comprehensive studies on solar storm: . Beijing: Center for Space Science and Applied Research, Chinese Academy of Sciences, 2007 (in Chinese) 谢妍琼.太阳风暴的综合研究: .北京:中国科学院空间科学与应用研究中心,2007

[12] Akasofu SI, Fry CF. A first generation numerical geomagnetic storm prediction scheme.Planetary Space Science, 1986, 34(1): 77~92

[13] Sun W, Akasofu SI. Calibration of the kinematic method of studying solar wind disturbances on the basis of a one-dimension MHD solution and a simulation study of the heliosphere disturbances between 22 November and 6 December 1977. Planetary Space Science, 1985, 33(8):933~943

[14] Fry CD, Sun W, Deehr CS, et al. Improvements to the HAF solar wind model for space weather predictions. Journal of Geophysical Research, 2001,106 (A10): 20985~21001

[15] Groth CPT, De Zeeuw DL, Gambosi TI, et al. Global 3-D MHD dimension of a space weather event: CME formation, interplanetary propagation, and interaction with the magnetosphere. Journal of Geophysical Research, 2000, 25: 25053~25078

用三维运动学模型研究行星际激波与共转高速流的相互作用

Interaction between interplanetary shock and corotating high speed stream studied by a 3-D kinematic method

PDF (PC)

可视化

摘要/Abstract

引用本文

使用本文

参考文献

相关文章 0

编辑推荐

Metrics

本文评价

访问统计

联系我们