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INTERFEROMETRIC SEEING MEASUREMENTS ON MT WILSON - POWER SPECTRA AND OUTER SCALES

机译：MT WILSON-功率谱和外部标尺的干涉测量

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We have measured power spectra of atmospheric phase fluctuations with the Mark. III stellar interferometer on Mt. Wilson under a wide variety of seeing conditions. On almost all nights, the high-frequency portions of the temporal power spectra closely follow the form predicted by the standard Kolmogorov-Tatarski model. At lower frequencies, a variety of behavior is observed. On a few nights, the spectra clearly exhibit the low-frequency flattening characteristic of turbulence with an outer-scale length of the order of 30 m. On other nights, examination of individual spectra yields no strong evidence of an outer scale less than a few kilometers in size, but comparison of the spectra on different interferometer baselines shows a saturation of the spatial structure function on long baselines. This saturation is consistent with the assumption of an outer-scale length similar to that derived for the nights when low-frequency flattening of the spectra is clearly seen. We discuss possible explanations of this behavior and conclude that power spectra from a single interferometer baseline are a poor diagnostic for the effective outer scale compared with multiple-baseline spectra. [References: 25]
机译：我们已经用Mark测量了大气相位波动的功率谱。三号恒星干涉仪在山。威尔逊在各种各样的观看条件下。在几乎所有夜晚，时间功率谱的高频部分都严格遵循标准Kolmogorov-Tatarski模型预测的形式。在较低的频率下，观察到各种行为。在几个晚上，光谱清楚地显示出湍流的低频展平特性，其外部尺度长度约为30 m。在其他夜晚，对单个光谱的检查并没有强有力的证据表明外部尺度小于几公里，但是在不同的干涉仪基线上对光谱进行比较显示，在长基线上空间结构功能饱和。当可以清楚地看到频谱的低频展平时，这种饱和度与假设类似于夜间导出的外部尺度长度的假设是一致的。我们讨论了这种行为的可能解释，并得出结论：与多基线光谱相比，来自单个干涉仪基线的功率光谱对有效外部尺度的诊断较差。 [参考：25]

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