Energy transport in the auroral ionosphere and magnetosphere

太阳风围绕地球磁层流动导致能量储存在热的电离气体或等离子体以及地球周围的磁场中。这种等离子体系统始于距地球约100公里的电离层，并将几十个地球半径延伸到太空中。由地球磁场控制的区域被称为磁层。极光显示是这种储存的能量释放到地球大气层和电离层上层的例子之一。该研究计划侧重于极光弧和极光或磁亚风暴这两种极光现象。该计划的项目包括对这些空间等离子体中能量传输的实验、理论和计算研究，主要推力有三个方向，包括超低频(ULF，1-10 MHz，100-1000 S周期)切变阿尔芬源、场线共振(FLR)、场线共振和极光弧物理，以及磁层和电离层亚暴物理。

The flow of the solar wind around the Earth's magnetosphere leads to the storage of energy in the hot ionized gas or plasma and the magnetic fields surrounding the Earth. This plasma regime starts about 100 km above the Earth in the ionosphere and extends many tens of Earth radii into space. The region dominated by Earth's magnetic field is called the magnetosphere. Auroral displays are one of the examples of the release of this stored energy into the upper regions of the Earth's atmosphere and ionosphere. The research program focuses on two auroral phenomena, the auroral arc and the auroral or magnetic substorm. Projects in the program include experimental, theoretical, and computational studies of the energy transport in these space plasmas, with major thrusts in three directions, including the sources of ultralow frequency (ULF, 1-10 mHz, 100-1000 s period) shear Alfven, field line resonances (FLRs), the physics of FLRs and auroral arcs, and the physics of substorms in the magnetosphere and ionosphere.