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太阳冠状热的区域中的三维磁场拓
1Max-Planck-Institut für Aeronomie, 37191 Katlenburg-Lindau, Germany. solanki@linmpi.mpg.de
Nature
|October 17, 2003
概括
科学家测量了太阳活动区域中的磁场,揭示了对太阳耀斑和冠状热的关键电流板. 这些发现支持了关于太阳大气中磁能消散的理论.
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:
- 太阳耀斑和X射线喷射源于与周围磁场相互作用的新兴磁流的活跃区域.
- 假设这些相互作用发生在电流板中,这些板对于冠状热至关重要.
- 这些电流板的复杂磁性结构在历史上使得它们难以测量.
研究的目的:
- 在日冕底部附近的太阳相互作用区域中确定全磁向量.
- 提供支持电流板在太阳活动和冠状热中的作用的观测证据.
主要方法:
- 在现场测量完整的磁向量.
- 在太阳冠冕底部观测一个活跃区域.
主要成果:
- 该研究成功确定了太阳相互作用区域中的完整磁场向量.
- 确定了两个关键的磁性特征:上升的磁环和磁场方向的接触性不连续性.
- 触点不连续性作为电流表的直接观察特征.
结论:
- 这些发现为基于电流板中的磁能消散的冠状热模型提供了强有力的观测支持.
- 这项研究推动了我们对驱动太阳耀斑和X射线喷射的物理过程的理解.
- 在这些地区测量磁场的能力为研究太阳动力学开辟了新的途径.
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