當行星際磁場發生變動時，太陽風與磁層的交互作用造成磁層結構的改變，而磁層與電離層是耦合在一起，高緯度電離層的沈降粒子能量與通量也因此而受到改變，所以我們可以藉由高緯度電離層的沈降粒子分布和變化，間接了解磁層中電漿和磁場環境的變動。在這個計畫中，我們將使用SuperMAG地磁資料庫所提供的SML指數，來分別判別地磁擾動時期和非擾動時期，並結合多顆NOAA衛星資料，統計分析在不同擾動時期下高緯度電離層的各種能量之沈降粒子的地方時和緯度分布，此外我們也將分析不同行星際磁場條件下這些沈降粒子分布的差異。藉由這些沈降粒子分布和變化的研究，我們對於磁層中的許多物理機制會有更進一步的了解。 ;When the interplanetary magnetic fields (IMF) vary, the interaction between the solar wind and magnetosphere will affect the magnetospheric configuration. Because of the coupling of the magnetosphere and ionosphere, the energy and flux of precipitating particles of the high-latitude ionosphere will be subsequently affected. Therefore, investigating the particle distributions and variations of the high-latitude ionosphere can help us indirectly understand the associated variations in the magnetosphere. In this study, we will use the SML geomagnetic index provided by the SuperMAG database to identify disturbed and non-disturbed periods. We will then statistically analyze the local time and latitudinal distributions of various energy channels of precipitating particles obtained from multiple NOAA satellites. We will also separate the data into various IMF conditions to understand the differences of the distributions. Through the distributions and variations of the precipitating particles in the high-latitude ionosphere, we can have some further understanding of physical mechanisms that occur in the magnetosphere.
