• ISSN 2097-1893
  • CN 10-1855/P

低高度极尖区位形的经验模式

刘子谦 李晖 王赤 韩金鹏 王江燕

引用本文: 刘子谦,李晖,王赤,韩金鹏,王江燕. 2022. 低高度极尖区位形的经验模式. 地球与行星物理论评(中英文),53(0):1-10
Liu Z Q, Li H, Wang C, Han J P, Wang J Y. 2022. Empirical model of the Earth's cusp at low-altitudes. Reviews of Geophysics and Planetary Physics, 53(0): 1-10 (in Chinese)

低高度极尖区位形的经验模式

doi: 10.19975/j.dqyxx.2022-044
基金项目: 国家自然科学基金资助项目(42022032,41874203,42188101);科工局民用航天预先研究项目(D020301,D030202);中科院先导专项项目(XDA17010301);中国科学院国际伙伴计划资助项目(183311KYSB20200017);中国科学院前沿科学重点研究计划(QYZDJ-SSW-JSC028);国家重点实验室专项研究基金资助项目
详细信息
    作者简介:

    刘子谦(1984-),男,助理研究员,主要从事磁层物理和空间天气的研究. E-mail:liuziqian@nssc.ac.cn

    通讯作者:

    李晖(1985-),男,研究员,主要从事行星际物理、磁层物理和空间天气等方面的研究. E-mail:hli@nssc.ac.cn

  • 中图分类号: P352

Empirical model of the Earth's cusp at low-altitudes

Funds: Supported by the National Natural Science Foundation of China (Grant Nos. 42022032, 41874203, 42188101), the project of Civil Aerospace Preliminary Research in Space Science (Grant Nos. D020301, D030202), the Strategic Priority Research Program of CAS (Grant No. XDA17010301), the International Partnership Program of CAS (Grant No. 183311KYSB20200017) , the Key Research Program of Frontier Science of CAS (Grant No. QYZDJ-SSW-JSC028), and the Special Research Fund of State Key Laboratories.
  • 摘要: 地球极尖区是太阳风等离子体进入内磁层和电离层的一个重要“窗口”,但其总体结构长期以来尚未确定. 2008年3月8日两个连续亚暴期间,太阳风的整体变化范围较大,基于全球三维数值模拟我们建立了一个由行星际磁场(interplanetary magnetic field, IMF)BYBZ控制的低高度(1.1个地球半径高度)极尖区的预报模式. 该模式由椭圆函数构造而成,拟合函数由极尖区位置和宽度控制并取决于IMF BYBZ. 极尖区地磁纬度(geomagnetic latitude, MLAT)随着向北IMF BZ的增加而增加,随着向南IMF BZ的增加而明显降低. 当BY=0时,磁地方时(magnetic local time, MLT)接近12,当IMF为东向(西向)时,极尖区中心将位于北半球下午(上午)侧. MLAT宽度随IMF BZ从北转南而减小,MLT宽度随IMF BZ从北转南而增大. 通过与DMSP卫星观测结果的比较分析,验证了该模型的有效性. 基于低高度极尖区预报模式,将进一步建立极尖区三维预报模式,这将有助于空间天气预报.

     

  • 图  1  2008年3月8日连续两次亚暴的概述. AU:虚线;AL:点线

    Figure  1.  The overview of two successive substorm on 8 March 2008

    图  2  北半球热压的空间分布. (a)西向IMF BY和南向BZ;(b)东向IMF BY和北向 BZ. 菱形表示极尖区中心,实线表示极尖区边界. BS:南向BZBN:北向BZP:热压

    Figure  2.  The spatial distribution of P on the northern hemispheric surface derived from the simulation data. The left panel shows that at 12:00 UT under dawnward IMF BY and southward BZ and the right panel shows that at 14:20 UT under duskward IMF BY and northward BZ. The cusp centers are denoted by diamonds, and the cusp boundaries are represents by solid lines

    图  3  北向(上)和南向(下)IMF时,判断得到的极尖区边界(菱形)和拟合结果(直线)

    Figure  3.  Two identified cusp boundaries (diamonds) and the corresponding curve fitting results (line) under northward and southward IMF

    图  4  事件期间极尖区拟合的相关系数分布,阈值由垂直虚线表示. mean:平均值,median:中值

    Figure  4.  The correlation coefficient distribution of the cusp fitting during the event. The threshold value is denoted by the vertical dashed line

    图  5  极尖区MLAT和MLT随IMF的变化(红线),并与Newell等(1989)(黑线)和Zhang等(2013)(黑线)对比

    Figure  5.  The comparison of our results (red line and red diamonds) with that given by Newell et al. (1989) (black line) and by Zhang et al. (2013) (black line)

    图  6  MLAT宽度和MLT宽度随IMF BZ的变化

    Figure  6.  The relation of MLAT width and MLT width with IMF BZ. The red lines are the fitting Results

    图  7  IMF BZ(a)和IMF BY(b)变化时,模式计算得到的极尖区边界

    Figure  7.  The cusp boundaries calculated from our 2-D cusp model under different IMF BZ (a) and IMF BY (b)

    图  8  (a, b)从DMSP观测到的沉降电子能量通量和观测到的极尖区(菱形);(c, d)极尖区模式结果和对应观测结果(菱形)的比较. eeflx:下行电子能量通量

    Figure  8.  (a, b) Time variation of the downward electron energy flux (line) and observed cusps (diamond) from the DMSP observations; (c, d) The comparison of the observed cusp (diamond) and predicted cusp (line) for the corresponding comment

    图  9  极尖区MLAT(a)和MLT(b)位置(实线)和宽度(灰色区域)随时间的演化,并与DMSP观测数据(菱形)对比

    Figure  9.  The time variation of the predicted cusp MLAT (a) and MLT (b) location (solid line) and width (grey zone), compared with the observed cusps from the DMSP observations (diamonds)

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出版历程
  • 收稿日期:  2022-05-12
  • 录用日期:  2022-05-23
  • 修回日期:  2022-05-22
  • 网络出版日期:  2022-06-06

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