由星际边界探测器对星际H,He和O进行直接观测
E Möbius1, P Bochsler, M Bzowski
1Space Science Center and Department of Physics, University of New Hampshire, Durham, NH 03824, USA. Eberhard.moebius@unh.edu
概括
当地的星际介质.
科学领域:
- 空间物理 空间物理
- 太空物理学 太空物理学
- 星际介质 星际介质
背景情况:
- 内部太阳系被来自当地的星际介质的中性气体透.
- 这种气体受到太阳引力和电离过程的影响.
- 能量中性原子 (ENA) 观测为这些相互作用提供了洞察力.
研究的目的:
- 分析太阳系内部星际,和氧的流动.
- 了解这些气体的时间变化和空间分布.
- 为了研究太阳引力和辐射压力对星际气体动态的影响.
主要方法:
- 使用来自星际边界探测器 (IBEX) 卫星的数据.
- 分析低能量的能量中性原子的全天空地图.
- 将观察到的流动模式与引力偏移和电离化的模型进行比较.
主要成果:
- 气和氧气的流量在2009年2月初达到峰值,这与引力偏移相一致.
- 2009年3月下旬之后,流成为主导,平衡了重力吸引与太阳辐射压力.
- 星际气体流源于日食平面上方,和氧气的温度相似.
- 不对称的氧气分布表明,来自外层的二次成分来自外层的二次成分.
结论:
- 太阳的重力和辐射压力在很大程度上影响了恒星间气体在日球内部的流动.
- 由于不同相互作用,IBEX的观测显示了,和氧的不同行为.
- 证据表明,存在复杂的星际环境,外层日光层的潜在贡献.
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