Auroral Phenomenology and Magnetospheric Processes: Earth And Other Planets - Keiling/Auroral Phenomenology and Magnetospheric Processes: Earth And Other Planets
Auroral Phenomenology and Magnetospheric Processes: Earth And Other Planets - Keiling/Auroral Phenomenology and Magnetospheric Processes: Earth And Other Planets
复制标题
极光现象学和磁层过程：地球和其他行星 - Keiling/极光现象学和磁层过程：地球和其他行星
DOI：
10.1029/2011gm001161
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发表时间：
2012
期刊：
影响因子：
--
通讯作者：
Lanchester B
中科院分区：
文献类型：
--
作者：
Lanchester B
极光的结构非常丰富（在磁场中的尺度可达数十米），运动速度快，颜色变化大。过去几十年开发的方法使用光谱信息，通过极光高层大气建模，来研究沉淀电子能量输入的变化以及对成分的依赖性，特别是原子氧变化。这些方法不仅在场对准光束的1-D区域，而且在磁天顶周围的更大的3-D区域中获得了关于极光现象的物理学的重要见解。本章回顾并描述了极光（前向）建模的最重要的细节，并展示了最新方法的功能和鲁棒性。这些方法将联合收割机排放率比与建模相结合，以估计初级降水粒子分布的能量。使用这种方法与测量的多光谱成像仪极光结构和动力学的重要结果被描述为概述的方法的例子。
The aurora is fascinatingly rich in structure (down to scale sizes of tens of meters across the magnetic field), with fast motions and change of color. Methods developed over the past several decades have used spectral information, with modeling of the auroral upper atmosphere, to study the changes in energy input of the precipitating electrons and the dependence on composition, in particular atomic oxygen variations. Important insight about the physics of auroral phenomena is obtained with these methods not only in the 1-D region of the field-aligned beam but in a larger 3-D region around the magnetic zenith. This chapter reviews and describes the most important details of (forward) modeling of the aurora and demonstrates the power and robustness of the latest methods. These methods combine emission rate ratios with modeling to estimate the energy of the primary precipitating particle distributions. Important results using such methods with measurements from the multispectral imager Auroral Structure and Kinetics are described as examples of the methods outlined.