GEM: Study of Solar Wind-Magnetosphere-Ionosphere Coupling

这项拟议的调查研究的能量和动量流 利用磁层顶的磁场原位观测 由ISEE 1和2号航天器获得的电场和等离子体， IGS磁强计链的地面数据。 平均 当行星际行星撞击地球时， 磁场是向南的，将使用这两个测量 垂直于磁层顶表面的磁场和气流 沿表面的沿着速度。 通过重复的个体测量 在整个表面上，重连场区域和 可以估计总的电位降。 为了确定 法向分量的三维形状的精确模型， 磁层顶将被导出。 这种压力依赖性 模型将允许我们测试压力脉冲是否会导致陨石坑 FTE的建议。 当IMF向北且重连较弱时， 传递仍然可以通过波过程进行。 我们将研究 从Pc 3到Pc 5周期出现的波，以确定是否 显著的波能通量穿过边界。 我们将研究 IGS磁强计链的同时地面数据， 2.5秒的分辨率，以确定波能量如何传播 磁层 我们还将研究极光的反应， 和亚极光带电流系统对动态压力变化的响应。 最后，我们将检查内部的每个边界层， 以确定它们中的每一个如何依赖于 太阳风的条件和磁层顶的位置， 确定哪些过程对这些边界层负责。 特别是，我们将研究它们的形成作为一个功能， 太阳风条件

This proposed investigation examines energy and momentum flow across the magnetopause using in-situ observations of magnetic field and plasmas obtained by the ISEE 1 and 2 spacecraft and ground based data from the IGS magnetometer chain. The average potential drop across the magnetosphere when the interplanetary magnetic field is southward will be measured using both the magnetic field normal to the magnetopause surface and the flow velocity along the surface. By repeated individual measurements across the surface, both the region of reconnected field and the total potential drop can be estimated. In order to determine the normal component an accurate model of the 3-D shape of the magnetopause will be derived. The pressure dependence of this model will allow us to test if pressure pulses can cause crater FTE's as has been suggested. When the IMF is northward and reconnection is weak, energy transfer can still take place by wave processes. We will examine the waves present from Pc 3 to Pc 5 periods to determine if significant wave energy flux crosses the boundary. We will examine simultaneous ground based data from the IGS magnetometer chain at 2.5s resolution to determine how this wave energy spreads through the magnetosphere. We will also examine the response of auroral and subauroral zone current systems to dynamic pressure changes. Finally, we will examine each of the boundary layers inside and outside the magnetosphere to determine how each of them depends on solar wind conditions and position on the magnetopause in order to determine what processes are responsible for these boundary layers. In particular we will examine their formation as a function of solar wind conditions.