Constructing the magnetospheric model including pressure measurements
Constructing the magnetospheric model including pressure measurements
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DOI：
10.1029/2001ja900167
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发表时间：
2002-06
影响因子：
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通讯作者：
M. Kubyshkina;V. Sergeev;S. Dubyagin;S. Wing;P. Newell;Wolfgang Baumjohann;A. Y. Liu
中科院分区：
文献类型：
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作者：
M. Kubyshkina;V. Sergeev;S. Dubyagin;S. Wing;P. Newell;Wolfgang Baumjohann;A. Y. Liu
[1]我们根据三个磁层探测器(AMPTE/IRM、AMPTE/CCE和ISEE1)的数据和DMSP航天器测量的质子降水，模拟了1985年4月19日高度扰动期间的磁尾构型。目的是测试在构建磁尾磁场模型时将等离子体压力作为输入数据的过程。根据AMPTE/IRM的数据，我们在统计上证实了尾部等离子体片在8-17RE距离处存在高度的各向同性压力，这使得从磁层磁场模型计算等离子体压力和沿相应的通量管的压力图变得容易。压力数据的使用不仅增加了面向事件建模的数据量，而且对磁层和电离层之间的构型和映射施加了非局部约束，使反问题的解更稳定，更接近实际。观测和模拟结果表明，观测到的构型与标准模型(T89或T96)的预测有很大的系统偏差[Tsyganenko，1989,1995]，并揭示了高度可变的构型，证明了发展面向事件的建模的必要性。在数据覆盖率最好的模式中，在12RE附近获得了局域化的B最小值和电流密度最大值，但该区域的降水没有显示出离散结构的特征。这种结构降水主要出现在极光带降水的极地半部，它被映射到较远的等离子体片部分(>；30RE)。
[1] We modeled the magnetotail configuration during a highly disturbed period on 19 April 1985 based on data from three magnetospheric spacecraft (Active Magnetospheric Tracer Explorers (AMPTE)/IRM, AMPTE/CCE, and ISEE 1) and proton precipitation measured by DMSP spacecraft. The goal was to test the procedure of including the plasma pressure as input data when constructing the magnetotail magnetic field model. On the basis of AMPTE/IRM data we confirm statistically a high degree of pressure isotropy at 8–17 RE distances in the tail plasma sheet, which allows computation of the plasma pressure from magnetospheric magnetic field model and easy mapping of the pressure along the corresponding flux tubes. The usage of pressure data not only increases the amount of data for event-oriented modeling but also imposes the nonlocal constraints on the configuration and mapping between magnetosphere and ionosphere to stabilize the solution of inverse problem and get it to be more realistic. Observational and modeling results indicate large systematic deviations of observed configuration from predictions of standard models (T89 or T96) [Tsyganenko, 1989, 1995] and reveal highly variable configurations, justifying a need for the development of event-oriented modeling. Indications of localized B minimum and current density maximum at around 12 RE have been obtained in the model with best data coverage, but precipitation from this region showed no signatures of discrete structures. The structured precipitation has been mostly seen in poleward half of the auroral zone precipitation, which is mapped to rather distant parts (>30 RE) of the plasma sheet.