Max Planck Institute for Solar System Research, 37077 Göttingen, Germany
Philos Trans A Math Phys Eng Sci. 2015 May 28;373(2042). doi: 10.1098/rsta.2015.0055.
The upper atmosphere of the Sun is governed by the complex structure of the magnetic field. This controls the heating of the coronal plasma to over a million kelvin. Numerical experiments in the form of three-dimensional magnetohydrodynamic simulations are used to investigate the intimate interaction between magnetic field and plasma. These models allow one to synthesize the coronal emission just as it would be observed by real solar instrumentation. Large-scale models encompassing a whole active region form evolving coronal loops with properties similar to those seen in extreme ultraviolet light from the Sun, and reproduce a number of average observed quantities. This suggests that the spatial and temporal distributions of the heating as well as the energy distribution of individual heat deposition events in the model are a good representation of the real Sun. This provides evidence that the braiding of fieldlines through magneto-convective motions in the photosphere is a good concept to heat the upper atmosphere of the Sun.
太阳的高层大气受磁场的复杂结构所支配。磁场控制着日冕等离子体加热到超过一百万开尔文的温度。以三维磁流体力学模拟的形式进行数值实验，用于研究磁场和等离子体之间的紧密相互作用。这些模型允许人们综合日冕发射，就像用真正的太阳仪器观察到的那样。涵盖整个活动区的大规模模型形成了与日冕极紫外光观测到的性质相似的演化日冕环，并再现了许多平均观测到的量。这表明，加热的空间和时间分布以及模型中单个热沉积事件的能量分布是对真实太阳的很好的表示。这表明，通过光球层中的磁对流转动对场线进行编结是加热太阳高层大气的一个很好的概念。
