Ion Energization and Escape on Mars and Venus
Ion Energization and Escape on Mars and Venus
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DOI：
10.1007/s11214-011-9831-7
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发表时间：
2011-10
影响因子：
10.3
通讯作者：
E. Dubinin;M. Fraenz;A. Fedorov;R. Lundin;N. Edberg;F. Duru;O. Vaisberg
中科院分区：
文献类型：
--
作者：
E. Dubinin;M. Fraenz;A. Fedorov;R. Lundin;N. Edberg;F. Duru;O. Vaisberg
火星和金星没有全球磁场，因此太阳风直接与它们的电离层和高层大气相互作用。太阳紫外线电离的中性原子，电荷交换和电子碰撞，被太阳风提取和清除，提供了行星挥发物的显着损失。电离的行星物质通过不同的渠道和路线逃离行星。由太阳风直接强迫驱动的离子迁移过程和它们的逃逸过程是密切相关的。不同通道中离子逃逸的力不同，相应地，逃逸的有效性也不同。火星和金星上的对流过程和逃逸通道的分类以及它们随太阳风参数的变化是我们评论的主要主题。我们将区分经典的皮卡和“质量加载”皮卡过程中，在边界层和等离子体片，极风与磁化电离层和增强逃逸流从局部极光区的强地壳磁场填充的地区未磁化的行星。
Mars and Venus do not have a global magnetic field and as a result solar wind interacts directly with their ionospheres and upper atmospheres. Neutral atoms ionized by solar UV, charge exchange and electron impact, are extracted and scavenged by solar wind providing a significant loss of planetary volatiles. There are different channels and routes through which the ionized planetary matter escapes from the planets. Processes of ion energization driven by direct solar wind forcing and their escape are intimately related. Forces responsible for ion energization in different channels are different and, correspondingly, the effectiveness of escape is also different. Classification of the energization processes and escape channels on Mars and Venus and also their variability with solar wind parameters is the main topic of our review. We will distinguish between classical pickup and ‘mass-loaded’ pickup processes, energization in boundary layer and plasma sheet, polar winds on unmagnetized planets with magnetized ionospheres and enhanced escape flows from localized auroral regions in the regions filled by strong crustal magnetic fields.