星际中性流通过日球界面的偏移
R Lallement1, E Quémerais, J L Bertaux
1Service d'Aéronomie du Centre National de la Recherche Scientifique, Institut Pierre Simon Laplace, Boite Postale 3, 91371 Verrières-le-Buisson, France. rosine.lallement@aerov.jussieu.fr
概括
星际气流与进入日球的气流相比,偏离了大约4度. 这种偏移表明星际磁场扭曲了日球,作为磁性指南针.
科学领域:
- * 太阳物理学和星际介质相互作用.
- *等离子体物理学和磁动力学.
背景情况:
- * 了解日球与星际介质 (ISM) 的相互作用对于太空天气和行星科学至关重要.
- * 之前的模型表明更简单的相互作用,没有显著的磁场影响中性气体流.
研究的目的:
- * 测量进入日球的中性流的精确方向.
- * 调查中性气体流中观察到的偏移的原因.
- * 利用和流向量来限制星际磁场方向.
主要方法:
- * 吸收细胞测量多普勒转移在星际共振发光.
- * 分析中性和的流向量在内部的日球.
主要成果:
- * 与流相比,中性流偏离了大约4度.
- *观察到的偏移与缺乏磁场效应的模型不一致.
- * 和流向量为星际磁场提供方向约束.
结论:
- * 周围的星际磁场显著扭曲了日球.
- * 中性流的偏移作为日球扭曲的指标.
- *混合和流向量作为一个有效的星际磁性指南针.
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