水平互联网磁场：数值模拟与Hinode观测的比较
The horizontal internetwork magnetic field: numerical simulations in comparison to observations with Hinode
摘要：
日之出空间天文台的观测结果是，在平静的互联网区域的光球层中发现了主要是水平的磁场。在这里，我们调查现实的数值模拟的太阳表面层相对于水平磁场和计算相应的偏振响应在Fe I 630 nm线对。我们发现一个局部最大值的水平场分量的平均强度在一个高度约500公里的光球，在那里它超过垂直分量的一个因素为2.0或5.6，这取决于初始和边界条件。从合成的斯托克斯配置文件，我们得到一个平均水平场分量，分别是1.6和4.3倍强于垂直分量。这是由于水平场本身的通量密度更强，并且水平场占据的面积更大。我们发现，对流过冲驱逐水平场的上层光球，使坡印亭通量为正的光球，而这个量是负的对流不稳定层下面。
英文摘要：
Observations with the Hinode space observatory led to the discovery of predominantly horizontal magnetic fields in the photosphere of the quiet internetwork region. Here we investigate realistic numerical simulations of the surface layers of the Sun with respect to horizontal magnetic fields and compute the corresponding polarimetric response in the Fe I 630 nm line pair. We find a local maximum in the mean strength of the horizontal field component at a height of around 500 km in the photosphere, where it surpasses the vertical component by a factor of 2.0 or 5.6, depending on the initial and boundary conditions. From the synthesized Stokes profiles we derive a mean horizontal field component that is, respectively, 1.6 and 4.3 times stronger than the vertical component. This is a consequence of both the intrinsically stronger flux density of, and the larger area occupied by the horizontal fields. We find that convective overshooting expels horizontal fields to the upper photosphere, making the Poynting flux positive in the photosphere, while this quantity is negative in the convectively unstable layer below it.
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