Simulation study on the Impulsive Electric Field induced by an interplanetary shock
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摘要:
行星际激波压缩地球磁层会产生全球尺度的脉冲电场, 这种脉冲电场进而会导致相对论电子发生快速的加速和注入行为, 因此脉冲电场的研究对内磁层的动力学问题的理解具有重要的意义.我们利用SWMF模型模拟了2015年12月19日的行星际激波事件, 来研究内磁层脉冲电场的演化和分布特性, 模拟结果表明: (1)脉冲电场主要沿环向向西; (2)脉冲电场在日侧的幅度普遍大于夜侧的幅度; (3)脉冲电场在日侧的持续时间普遍小于夜侧的持续时间.模拟结果中脉冲电场的特征与Zhang等人(2018)中基于范艾伦卫星数据的统计结果一致, 从而验证了统计结果的可靠性.这些结果将有助于对辐射带高能粒子对极端空间天气的快速响应的理解.
Abstract:As an interplanetary shock(IPS)compresses on the Earth's magnetosphere, it will launch impulsive electric fields in the inner magnetosphere, which may further induce prompt acceleration and injection of relativistic electrons. Thus, impulsive electric field could be important to the topic of dynamics in the inner magnetosphere. We perform a MHD simulation on magnetospheric response to interplanetary shock occurred in 2015 December 19th with the Space Weather Modeling Framework(SWMF), to investigate its characteristics on spatial distribution and temporal evolution. The result shows that: (1) impulsive electric field is induced mainly westward; (2) its amplitude in dayside is larger than it in nightside; (3) its rising time in dayside is shorter than it in nightside. The three main characteristics in simulation are consistent with the statistical results by Zhang et al. (2018) with Van Allen Probes measurements. These results will be helpful for the understanding the prompt response of high energy radiation belt particles to extreme space weather conditions.
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Key words:
- Interplanetary shock /
- MHD simulation /
- Space plasma /
- Inner magnetosphere
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图 1
Wind卫星在L1点测量的(a)质子密度、(b)太阳风速度GSE坐标下的X分量、(c)质子温度和(d)GSE坐标下磁场矢量观测数据以及(e)OMNI数据库的SYM-H指数.两个红色垂直虚线分别代表行星际激波依次到达日地L1点以及地球磁层的时间
Figure 1.
(a) Proton number density, (b) X component of solar wind velocity in GSE coordinate, (c) proton temperature and (f) magnetic field vector in GSE coordinate obtained from Wind spacecraft measurement at L1 point and (e) SYM-H index obtained from OMNI database. Two vertical dashed lines respectively represent the interplanetary shock′s arrival at the Sun-Earth L1 point and the Earth′s magnetosphere
图 2
范艾伦B卫星的轨道信息示意图，其中箭头代表卫星运行方向
Figure 2.
A schematic of the orbit information of Van Allen Probe-B, where arrows represent the direction of spacecraft motion
图 3
范艾伦B卫星的电磁场观测结果(左)和SWMF电磁场模拟结果(右).GSE坐标下电场的X和Y分量的数据(a—b和f—g)以及磁场的X、Y和Z分量数据(c—e和h—j).红色垂直虚线代表行星际激波导致的脉冲电场的起始时间
Figure 3.
Van Allen Probe-B observational results (left) and SWMF numerical result (right). (a—b and f—g) electric field X and Y components and (c—e and h—j) magnetic field X, Y and Z components in GSE coordinate. The red vertical dashed lines indicate the onset time of IPS-induced impulsive electric field
图 4
SWMF模拟结果中，行星际激波到达之后第一个脉冲电场的幅度和大小在赤道面的分布图.箭头长度和颜色代表脉冲电场幅度，右上图例展示了5 mV·m-1大小的脉冲电场对应的箭头长度，右侧的色标也可以作为幅度的参考，虚线圆作为L=2、4、6以及地球同步轨道的位置参考
Figure 4.
The amplitude and orientation of initial impulsive electric field after IPS′s arrivalst the Earth′s magnetosphere in the SWMF simulation result. Both length of arrows and color represent the amplitude of the impulsive electric field. The legend and color bar can both be a reference for the amplitude. The dashed circles are the references for the location of L=2, 4 and 6 and the geosynchronous orbit
图 5
SWMF模拟结果中L=5的高度上磁地方时分别为(a)12、(b)18和(c)24的位置的脉冲电场演化，从上至下分别为GSE坐标下X(蓝色)和Y(橙色)方向的电场以及环向(黑色)电场
Figure 5.
The impulsive electric field evolution in SWMF simulation result at the positions where MLT equals (a) 12, (b) 18 and (c) 0, respectively. From top to bottom, the electric fields in the X (blue) and Y (orange) directions and the azimuthal (black) electric field in GSE coordinates, respectively
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