Space Weather: MHD and Empirical Magnetosheath Models

研究人员将为大范围的太阳风参数和真实的磁层顶形状开发新一代磁鞘模型。许多太阳风-磁层相互作用的研究都需要磁鞘参数的定量模型。需要这样的模型来确定太阳风特征到达的时间，确定磁层顶的条件是否有利于重联，以及描述输入到尖端和地幔的磁鞘等离子体参数。现有的模型仅有的是忽略磁场的气体动力学模型。研究人员将开发一种基于磁流体动力学(MHD)的新模型。该模型的结果将与现有的气体动力学模型以及根据现场卫星数据开发的经验模型进行比较。研究结果还将被用来区分日侧磁层顶上各种拟议的磁合并模式。MHD磁鞘模型将有助于更好地理解太阳风-磁层-电离层系统中的等离子体过程和能量转移，并有助于评估由于太阳风和行星际磁场的变化而导致的陆地环境变化。

ATM9819705absSimon WingThe investigators will develop a new generation magnetosheath model for a wide range of solar wind parameters and realistic magnetopause shapes. Many studies of the solar wind-magnetosphere interaction require quantitative models for magnetosheath parameters. Such models are needed to time the arrival of solar wind features, determine whether conditions at the magnetopause are favorable for reconnection, and to describe the magnetosheath plasma parameter input into the cusp and mantle. The only existing models are gas dynamic models which neglect the magnetic field. The investigators will develop a new model based on magnetohydrodynamics (MHD). The results of this model will be compared to existing gas dynamic models and to empirical models developed from in situ satellite data. The results will also be used to discriminate between various proposed modes of magnetic merging on the dayside magnetopause. The MHD magnetosheath model will help improve the understanding of the plasma processes and energy transfer in the solar wind-magnetosphere-ionosphere system and help assess the terrestrial environmental variations due to changes in the solar wind and interplanetary magnetic field.