Studies of energization of magnetospheric particles by substorm dipolarizations

拟议研究的目标是模拟亚暴事件期间产生的高能粒子（主要是电子和质子）的通量。地球静止轨道上的卫星经常观测到这些粒子通量的增强与亚暴偶极有关。这些粒子通常具有数百keV的能量，并且能够损坏卫星电子设备，从而导致该行业的重大经济损失。尽管多年的积极研究，许多问题，有关的反渗透过程仍然没有答案。我们考虑了亚暴偶极的两种情形：偶极向拉伸磁力线跃迁的尾向传播边缘和向地球传播的电磁脉冲。这两种情况都导致了电子和质子尾部数量的显著增加，并且都有观测支持。第一种情况得到了地面观测的充分支持，如极光的光度计观测和电离层透射率的riometer观测，第二种情况得到了现场卫星观测的充分支持。我们的建模工作将有助于提高我们的带电粒子的磁层和电离层的磁层和电离层的影响的量化过程的理解。最终，我们希望能够量化这两种情况在空间和电离层中的表现。这将使我们能够区分两者，并调和地面观测和卫星观测之间的明显分歧。

The goal of the proposed research is to model the fluxes of energetic particles (mostly electrons and protons) generated during substorm events. Enhanced fluxes of these particles are often observed by satellites at geostationary orbit in association with substorm dipolarizations. These particles often possess energies of hundreds of keVs and are capable of damaging satellite electronics resulting in significant economic losses for the industry. Despite many years of active research many questions regarding the energization process remain unanswered. We consider two scenarios of substrom dipolarizations: the tailward propagating edge of the transition from dipole to stretched magnetic field lines and earthward propagating electromagnetic pulse. Both scenarios lead to significant energization of the tail populations of electrons and protons and both have observational support. The first scenario is well supported by the ground-based observations, such as photometer observations of auroras and riometer observations of the ionospheric transmissivity, the second by in-situ satellite observations. Our modeling efforts will help to improve our understanding of the energization process of the charged particles and quantify their effects in the magnetosphere and ionosphere. Ultimately, we hope to be able to quantify the manifestations of the two energization scenarios both in space and in the ionosphere. This will allow us to distinguish the two and to reconcile the apparent disagreement between the ground-based and satellite observations.