Aulanier Guillaume, Golub Leon, Deluca Edward E, Cirtain Jonathan W, Kano Ryouhei, Lundquist Loraine L, Narukage Noriyuki, Sakao Taro, Weber Mark A
Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie (UPMC), Université Paris Diderot, 92190 Meudon, France.
Science. 2007 Dec 7;318(5856):1588-91. doi: 10.1126/science.1146143.
Magnetic reconnection of solar coronal loops is the main process that causes solar flares and possibly coronal heating. In the standard model, magnetic field lines break and reconnect instantaneously at places where the field mapping is discontinuous. However, another mode may operate where the magnetic field mapping is continuous but shows steep gradients: The field lines may slip across each other. Soft x-ray observations of fast bidirectional motions of coronal loops, observed by the Hinode spacecraft, support the existence of this slipping magnetic reconnection regime in the Sun's corona. This basic process should be considered when interpreting reconnection, both on the Sun and in laboratory-based plasma experiments.
太阳日冕环的磁重联是引发太阳耀斑并可能导致日冕加热的主要过程。在标准模型中，磁力线在磁场映射不连续的位置瞬间断裂并重新连接。然而，在另一种模式下，磁场映射是连续的，但呈现出陡峭的梯度：磁力线可能会相互滑动。日地关系天文台（Hinode）航天器观测到的日冕环快速双向运动的软X射线观测结果，支持了太阳日冕中这种滑动磁重联机制的存在。在解释太阳和基于实验室的等离子体实验中的重联现象时，都应考虑这一基本过程。
