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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >New Diagnosis for Energy Flow From Solar Wind to Ionosphere During Substorm:Global MHD Simulation
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New Diagnosis for Energy Flow From Solar Wind to Ionosphere During Substorm:Global MHD Simulation

机译：从太阳风能量流的新诊断亚暴时电离层:全球磁流体动力模拟

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摘要

To investigate the energy involved by a substorm, we performed global magnetohydrodynamics simulation for different solar wind conditions. The intensity of the auroral electrojet increases with the southward component of interplanetary magnetic field (IMF) and the solar wind velocity, which is consistent with observations. To evaluate the energy that enters the magnetosphere, we first defined a solar wind effective cross-sectional area in which all the Poynting fluxes entering the magnetosphere pass through. We found that the solar wind magnetic energy is insufficient to provide the magnetic energy entering the magnetosphere (intake magnetic energy) for southward IMF. About 33-88% of the intake magnetic energy is converted from the solar wind kinetic energy. About 2-7% of the solar wind kinetic energy (passing through the effective area) is converted to the magnetic energy that enters the magnetosphere. Significant contribution from the solar wind kinetic energy makes the energy coupling function complicated. The effective area also depends on the solar wind parameters, also making it complicated. An interesting point is that the rates of energy stored and released in the lobe also depend on the solar wind parameters. The ionospheric Joule heating rate is well correlated with the intake magnetic energy at onset, and during the substorm expansion. The correlation coefficients between them are better than that of the ε parameter. These results imply that both the directly driven process (manifested by intake magnetic energy) and loading-unloading process (manifested by stored/released energy in the lobe) are largely regulated by the solar wind condition.
机译：调查涉及的能量由亚暴,我们执行全球磁动流体力学模拟不同的太阳风条件。极光电喷流的强度增加星际的向南的组成部分磁场(货币基金组织)和太阳风速度,这是与观测一致。评估的能量进入磁气圈,我们首先定义了太阳风所有的有效横截面积能流密度通量进入磁层通过通过。能量不足以提供磁能源进入磁层(摄入量磁能)向南国际货币基金组织(IMF)。摄入的磁能转换太阳风动能。太阳风动能(通过有效面积)转换为磁场能量进入磁层。从太阳风动能贡献使能量耦合功能复杂。还取决于太阳风的有效区域参数,也使它复杂。有趣的一点是,利率的能量叶也依赖于存储和释放太阳风参数。升温速率远与摄入量磁性能量爆发,在亚暴扩张。他们比ε的参数。这些结果暗示了直接驱动的过程(通过磁性能量摄入)和装卸过程(体现存储/释放能量叶)在很大程度上由太阳风条件。

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