来自空间观测的安静太阳磁场：模拟Hinode的情况
Quiet Sun magnetic fields from space-borne observations: simulating Hinode's case
摘要：
我们研究是否有可能从非常高的空间分辨率的偏振观测在可见光得到安静的太阳互联网区域的场强分布。特别是，我们考虑的情况下，分光偏振仪连接到太阳光学望远镜登上日之出。辐射磁对流模拟被用来合成四个斯托克斯轮廓的\ion{Fe}{1} 630.2 nm线。一旦配置文件被降级到0 \farcs 32的空间分辨率和添加的噪声，我们推断的大气参数通过米尔恩-爱丁顿反演。与真实值的比较表明，可见线产生正确的网络间的磁场强度和磁通量，与不确定性小于$\sim$ 150 G，杂散光污染因子时，包括在反演。与1 \arcsec的地基观测结果相反，在模拟中，只要磁场弱，就可以恢复弱场。
英文摘要：
We examine whether or not it is possible to derive the field strength distribution of quiet Sun internetwork regions from very high spatial resolution polarimetric observations in the visible. In particular, we consider the case of the spectropolarimeter attached to the Solar Optical Telescope aboard Hinode. Radiative magneto-convection simulations are used to synthesize the four Stokes profiles of the \ion{Fe}{1} 630.2 nm lines. Once the profiles are degraded to a spatial resolution of 0\farcs32 and added noise, we infer the atmospheric parameters by means of Milne-Eddington inversions. The comparison of the derived values with the real ones indicates that the visible lines yield correct internetwork field strengths and magnetic fluxes, with uncertainties smaller than $\sim$150 G, when a stray light contamination factor is included in the inversion. Contrary to the results of ground-based observations at 1\arcsec, weak fields are retrieved wherever the field is weak in the simulation.
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