The Magnetic Field Structure in the Heliosheath
The Magnetic Field Structure in the Heliosheath
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日鞘中的磁场结构
DOI：
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发表时间：
2005
期刊：
影响因子：
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通讯作者：
J. Jokipii
中科院分区：
文献类型：
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作者：
J. Jokipii
在波动的、动态的日鞘中观测到的磁场与静态的日鞘中观测到的磁场有很大的不同。特别是，电流片交叉（部门）之间的时间是相当敏感的太阳风终端冲击的径向速度。如果一个向内移动的终端激波从一个缓慢移动的航天器上的观测者身边经过，那么在合理预期的向内激波速度下，日鞘中电流片交叉之间的时间会变得更长，并且可能变得非常大。这种效应可能有助于解释最近从旅行者1号宇宙飞船上观测到的磁场，在日鞘中，磁场已经从太阳向外定向了几个月。
The magnetic field observed in a fluctuating, dynamical heliosheath will differ considerably from that in a static heliosheath. In particular, the time between current-sheet crossings (sectors) is quite sensitive to the radial speed of the solar wind termination shock. If an inwardly moving termination shock moves past an observer on a slowly moving spacecraft, the time between current-sheet crossings in the heliosheath becomes larger, and can become very large, for reasonably expected inward shock speeds. This effect may help to explain recent observations of the magnetic field from the Voyager 1 spacecraft, where, in the heliosheath, the magnetic field has remained directed outward from the Sun for several months.