Studies of energization of magnetospheric particles by substorm dipolarizations

提出的研究目标是模拟在亚暴事件中产生的高能粒子（主要是电子和质子）的通量。在地球静止轨道上的卫星经常观测到这些粒子的增强通量与亚暴极化有关。这些粒子通常具有数百千伏的能量，能够破坏卫星电子设备，给工业造成重大的经济损失。尽管经过多年的积极研究，许多关于能量化过程的问题仍未得到解答。我们考虑了两种情况：从偶极子到拉伸磁力线过渡的尾部传播边缘和向地球传播的电磁脉冲。这两种情况都导致电子和质子尾部居群的显著能量化，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，例如光度计对极光的观测和电离层透射率的日冕仪观测，第二种情况得到了原位卫星观测的支持。我们的建模工作将有助于提高我们对带电粒子的通电过程的理解，并量化它们在磁层和电离层中的影响。最终，我们希望能够量化在空间和电离层中两种能量情景的表现。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明显的分歧。

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.