Energy transport in the auroral ionosphere and magnetosphere

太阳风在地球磁层周围的流动导致能量储存在热电离气体或等离子体和地球周围的磁场中。 这种等离子体状态开始于地球上方约100公里的电离层中，并延伸到数十个地球半径的太空中。 由地球磁场主导的区域称为磁层。 极光的出现是这种储存的能量释放到地球大气层和电离层上部的例子之一。 该研究计划的重点是两种极光现象，极光弧和极光或磁亚暴。 该计划中的项目包括这些空间等离子体中能量传输的实验，理论和计算研究，主要推力在三个方向，包括超低频（ULF，1-10 mHz，100-1000 s周期）剪切阿尔芬，场线共振（FLR），FLR和极光弧的物理学，以及磁层和电离层亚暴的物理学。

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.