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IMF北向时太阳风粒子向磁层输运的试验粒子模拟研究

赵明现

赵明现. IMF北向时太阳风粒子向磁层输运的试验粒子模拟研究[J]. 空间科学学报. doi: 10.11728/cjss2022.06.210721078
引用本文: 赵明现. IMF北向时太阳风粒子向磁层输运的试验粒子模拟研究[J]. 空间科学学报. doi: 10.11728/cjss2022.06.210721078
ZHAO Mingxian. Test Particle Simulation of Solar Wind Transport into the Magnetosphere during Northward IMF (in Chinese). Chinese Journal of Space Science, xxxx, x(x): x-xx doi: 10.11728/cjss2022.06.210721078
Citation: ZHAO Mingxian. Test Particle Simulation of Solar Wind Transport into the Magnetosphere during Northward IMF (in Chinese). Chinese Journal of Space Science, xxxx, x(x): x-xx doi: 10.11728/cjss2022.06.210721078

IMF北向时太阳风粒子向磁层输运的试验粒子模拟研究

doi: 10.11728/cjss2022.06.210721078
基金项目: 国家自然科学基金项目资助(42274217,41774195)
详细信息
    作者简介:

    赵明现:E-mail:zhaomx@cma.gov.cn

  • 中图分类号: P353

Test Particle Simulation of Solar Wind Transport into the Magnetosphere during Northward IMF

  • 摘要: 以ACE卫星实时观测数据驱动的全球磁流体模拟为背景场,选取2003年10月22-24日行星际磁场(IMF)持续北向的事件,使用试验粒子方法,对太阳风粒子向磁层输运的过程进行模拟研究,分析北向IMF下太阳风粒子注入磁层过程中粒子在磁层内的空间分布和时间演化特征。IMF北向期间,进入环电流区域的粒子在晨侧区域的密度大于昏侧,且晨侧的粒子分布范围更广。背阳面磁鞘中的太阳风粒子可以通过低纬边界层进入磁层,但很难通过南北侧磁层顶进入磁层。进入磁尾的太阳风粒子聚集形成冷而密的等离子体片(CDPS),模拟中CDPS的空间分布和密度大小与观测数据符合。在IMF长时间北向期间,磁尾的粒子数量呈现随时间增长的趋势,并存在约20 min的小幅度准周期变化和约5~6 h的较大幅度的准周期变化。

     

  • 图  1  2003年10月22-25日ACE卫星观测到的太阳风和IMF数据

    Figure  1.  ACE satellite observation data on 22-25 October 2003

    图  2  使用不同时间步长计算得到的粒子运动轨迹

    Figure  2.  Trajectories of a single particle using different settings of time step

    图  3  Geotail卫星观测粒子密度与模拟结果对比

    Figure  3.  Comparison between the particle density observed by Geotail and that from our simulation

    图  4  太阳风粒子在磁层中的三维密度分布(黑色实线为磁层顶位置,白色实线为弓激波位置)

    Figure  4.  Three dimensional density distribution of solar wind particles in magnetosphere (black solid lines mark the location of magnetopause, and the white solid lines mark the location of bow shock)

    图  5  太阳风粒子在磁层中的三维密度分布

    Figure  5.  Three dimensional density distribution of solar wind particles in magnetosphere

    图  6  太阳风粒子在xy平面的密度分布

    Figure  6.  Density distribution of solar wind particles on xy plane

    图  7  太阳风粒子在xz平面的密度分布,

    Figure  7.  Density distribution of solar wind particles on xz plane

    图  8  太阳风粒子在 x = –20 Re处的yz平面的密度分布

    Figure  8.  Density distribution of solar wind particles on yz plane at x = –20 Re

    图  9  磁尾选定区域(–40 Re < x < –10 Re , –15 Re < y < 15 Re , –10 Re < z < 10 Re )内的粒子平均密度和密度最大值在IMF北向期间随时间的变化

    Figure  9.  Variation of total particle average density and particle max density maximum during northward IMF in the selected magnetotail region (–40 Re < x < –10 Re , –15 Re < y < 15 Re , –10 Re < z < 10 Re)

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    GUO Jiuling, SHEN Chao, LIU Zhenxing. Simulation of the cross sections of the magnetotail and particle transferred into the plasma sheet under north- and southward IMF conditions[J]. Chinese Science Bulletin, 2014, 59(4/5): 345-350 doi: 10.2360/972012-1852
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出版历程
  • 收稿日期:  2021-07-18
  • 录用日期:  2021-09-27
  • 修回日期:  2022-03-15
  • 网络出版日期:  2022-11-09

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