Structure and evolution of magnetic fields associated with solar eruptions
Structure and evolution of magnetic fields associated with solar eruptions
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DOI：
10.1088/1674-4527/15/2/001
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发表时间：
2014-12
影响因子：
1.8
通讯作者：
Haimin Wang;Chang Liu
中科院分区：
文献类型：
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作者：
Haimin Wang;Chang Liu
本文综述了太阳活动区光球磁场演化及其与耀斑关系的研究。它分为两个主题，导致太阳爆发的磁结构和演变以及与爆发有关的光球磁场的快速变化。对于第一个主题，我们描述了磁复杂性，新的通量出现，通量抵消，剪切运动，太阳黑子旋转和磁螺旋度注入，这可能都有助于存储和积累的能量，触发太阳爆发。对于第二个主题，我们集中在与耀斑相关的光球磁场的快速和不可逆变化的观测，以及对三维磁场重组的影响。我们特别强调光球磁场观测方面的最新进展，因为最先进的观测设施（如日之出和太阳动力学观测台）已经投入使用。在这一研究领域的观察，理论和未来的前景之间的联系进行了讨论。
This paper reviews the studies of solar photospheric magnetic field evolution in active regions and its relationship to solar flares. It is divided into two topics, the magnetic structure and evolution leading to solar eruptions and rapid changes in the photospheric magnetic field associated with eruptions. For the first topic, we describe the magnetic complexity, new flux emergence, flux cancelation, shear motions, sunspot rotation and magnetic helicity injection, which may all contribute to the storage and buildup of energy that trigger solar eruptions. For the second topic, we concentrate on the observations of rapid and irreversible changes of the photospheric magnetic field associated with flares, and the implication on the restructuring of the three-dimensional magnetic field. In particular, we emphasize the recent advances in observations of the photospheric magnetic field, as state-of-the-art observing facilities (such as Hinode and Solar Dynamics Observatory) have become available. The linkages between observations, theories and future prospectives in this research area are also discussed.