To reconcile discrepancies in the observed contrast of magnetic flux concentrations, we compute synthetic filtergrams from solar magnetoconvection models in four different passbands: two continuum bands, at 1626 and 575 nm, the G band, and the line wing of the Ca II K line. Magnetic flux concentrations are selected by their G-band brightness. In the near-infrared the selected flux concentrations appear inconspicuous with intensities that are on average below that of the synthetic average quiet Sun, while their contrast in the visible passband is mostly positive. When we account for limited telescope resolution and imperfect seeing, the contrasts of bright points in the visible become increasingly negative as a result of mixing with the dark intergranular lanes in which they are embedded. The correlation in bright-point intensity between different passbands becomes increasingly poor from the G band to the visible and the near-infrared. This is caused in part by the varying amount of spectral lines in each of the bands. Further, we find that the largest magnetic field concentrations, representative of micropores or magnetic knots, are dark in all four passbands. The brightenings in the Ca II K line wing do not coincide with magnetic flux concentrations on the spatial scale of the simulation. Finally, we find that the rms intensity contrast in all four passbands depends on the amount of magnetic field present in the simulation, with higher contrast for lower average magnetic field strength.
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机译：为了调和观测到的磁通量浓度差异，我们根据太阳磁对流模型在四个不同的通带中计算合成滤镜图：两个连续谱带（分别位于1626和575 nm），G谱带和Ca II K谱线的谱线。磁通量浓度由其G波段亮度选择。在近红外中，所选的通量浓度与平均低于合成平均安静太阳强度的强度相比并不明显，而它们在可见通带中的对比度通常为正。当我们考虑到有限的望远镜分辨率和不完美的视线时，由于与暗暗的晶界车道混合在一起，可见光中亮点的对比度变得越来越负。从G波段到可见光和近红外，不同通带之间的亮点强度相关性越来越差。这部分是由于每个频带中频谱线数量的变化引起的。此外，我们发现，在所有四个通带中，代表微孔或磁结的最大磁场浓度是暗的。 Ca II K线机翼中的增亮与模拟空间尺度上的磁通量浓度不一致。最后，我们发现所有四个通带的均方根强度对比度取决于仿真中存在的磁场量，较高的对比度则可降低平均磁场强度。
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