Test Particle Simulation of Solar Wind Transport into the Magnetosphere during Northward IMF
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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。Abstract: Using test particle method, with the background fields obtained from a global Magnetohydrodynamics (MHD) simulation driven by the ACE satellite observation data, the transport process of solar wind particles into the Earth’s magnetosphere was simulated during a long-term northward Interplanetary Magnetic Field (IMF) event on 22－24 October 2003. The particle density distribution in the magnetosphere and the time evolution characteristics of the particles were analyzed and discussed. During the northward IMF, the particle density in the dawn-side ring current region is higher than that on the dusk side, and the radial range on the dawn side is wider. The magnetosheath particles on the tail side can transport into magnetosphere through the low-latitude boundary layer, but they are difficult to enter into magnetosphere through the north and south magnetopause. The solar wind particles transported into the nightside magnetosphere gather to form a Cold Dense Plasma Sheet (CDPS). The spatial scale and particle density of the CDPS obtained from the simulation are consistent with observations. During the long-term northward IMF period, the total number of particles in the magnetotail showed a trend of increasing over time. At the same time, there exists a weak quasi-periodic variation with a period of about 20 min and a strong quasi-periodic variation with a period of about 5～6 h.
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Key words:
- Solar wind /
- Northward IMF /
- Magnetosphere /
- Test particle simulation
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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 in 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 in 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 in 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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