太阳冠冕中的能量释放来自空间分辨的磁
J W Cirtain1, L Golub, A R Winebarger
1Marshall Space Flight Center, NASA, Mail Code ZP13, MSFC, Alabama 36812, USA. jonathan.w.cirtain@nasa.gov
Nature
|January 25, 2013
概括
在太阳的冠冕中的磁重新连接将等离子体加热到几百万克尔文度. 新的高分辨率观测揭示了冠冕中的微型磁,为这种加热机制提供了证据.
科学领域:
- 太阳物理 太阳物理
- 等离子体天体物理学
- 磁动力学 磁动力学
背景情况:
- 太阳的外层大气 (冠状) 需要大量的加热,达到150万到400万克尔文的温度.
- 浪热用于安静的太阳能时期,但活跃的地区需要额外的能源.
- 编织磁场线的磁再连接是主动冠状热的领先理论候选者.
研究的目的:
- 为磁和重连接作为太阳冠状的加热机制提供观测证据.
- 为了解决新冠中以前未被观察到的微小磁性结构.
- 为了量化观察到的磁再连接事件释放的能量.
主要方法:
- 太阳活动区域的高分辨率成像,角分辨率为0.2弧秒.
- 观测和分析冠状体内的微型磁.
- 监测磁场重新连接,放松和能量消耗过程.
主要成果:
- 在太阳冠冕中直接观测微尺度磁 (0.2弧秒).
- 这些编织的磁结构的重新连接和放松的证据.
- 观察到的能量消散足以将冠状体等离子体加热到大约400万凯尔文.
结论:
- 微型子的磁性重新连接是加热活跃太阳冠状的可行机制.
- 从场放松中观察到的能量释放足以解释高温.
- 需要进一步的观察来证实这一机制是所有活跃区域中占主导地位的加热过程.
相关概念视频
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Magnetic field lines follow several hard-and-fast rules:
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