近太阳风中的阿尔夫尼克速度峰值和旋转流
J C Kasper1,2, S D Bale3,4,5, J W Belcher6
1Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA. jckasper@umich.edu.
Nature
|December 6, 2019
概括
超音速太阳风的加速是由阿尔夫恩波组织成结构化的速度尖峰驱动的. 这些尖峰揭示了太阳风中的重要旋转成分, 挑战了当前的恒星角动量损失模型.
科学领域:
- * 太空物理学和等离子物理学
- 太阳物理与恒星进化
背景情况:
- 在太阳附近超音速太阳风的加速得到证实,
- * 阿尔弗尼克波动是一个候选机制,在冠状和太阳风中观察到显著的能量.
- 之前的观测显示太阳风在远离太阳的区域内旋转的幅度很小.
研究的目的:
- 在大约35个太阳半径的日中心距离上研究太阳风等离子体动力学和能量传输.
- * 确定导致太阳风加速和太阳能向外传输的过程.
- * 评估太阳风流的旋转成分及其对恒星角动量损失的影响.
主要方法:
- 太阳风等离子体的现场观测,使用太空船在35太阳半径的日中心距离.
- *对阿尔夫恩波,磁场线和等离子体流速的分析.
- * 观察到的旋转速度与经典预测和波幅的比较.
主要成果:
- * 阿尔夫恩波组织成结构化的速度峰值 (持续时间长达几分钟),与S型磁场曲线相关.
- * 在太阳风流速中检测到一个显著的旋转组成部分,其峰值为3550公里/秒.
- * 观察到的旋转流量大大超过了几公里/秒的经典预测.
结论:
- * 这些发现挑战了现有的太阳风冠状循环和能量传输模型.
- * 重要的旋转元件表明恒星的角动量损失的机制更复杂.
- 了解这些过程对于理解恒星如何随着时间的推移而失去角动力和旋转至关重要.
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