从开放封闭的磁场结构中研究太阳风的输出流,使用协调太阳轨道仪和海诺德观测
Nawin Ngampoopun1, Roberto Susino2, David H Brooks3,1
1Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT UK.
概括
研究来自ESA/NASA的太阳风外流.
科学领域:
- 太阳物理 太阳物理
- 等离子体物理学的物理学
- 天体物理学 天体物理学
背景情况:
- 太阳冠冕是太阳风的来源.
- 了解太阳风的起源需要近距离观察和多视角的观点.
- 太阳轨道探测器 (SO) 任务为研究冠状病毒提供了前所未有的数据.
研究的目的:
- 分析和比较太阳风从一个狭窄的开放场走廊和一个中度冠状孔的流出.
- 为了研究等离子体属性和太阳冠冕中的磁场结构之间的关系.
- 了解太阳风变化的驱动因素.
主要方法:
- 通过Metis冠状图 (SO) 和极端紫外线成像光谱仪 (EIS) (Hinode) 的观察.
- 分析太阳风从离肢和盘上观测的输出流.
- 磁场推断以确定源区域.
主要成果:
- 来自开放场走廊的等离子体显示出较高的电子密度和较低的流出速度,而不是中部冠状病毒中的冠状孔等离子体.
- 低冠状的源区域表现出类似的等离子体特性.
- 来自开放场走廊的太阳风速度与磁场膨胀因子没有相关,与冠状孔不同.
结论:
- 高海拔地区等离子体特性上的差异表明,中低层冠状体中存在动态过程.
- 磁再连接可能在推动太阳风变化的过程中发挥重要作用.
- 太阳风的起源是复杂的,取决于特定的冠状结构和动态.
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