金星极化测量一百周年：PICSARR观测的相位曲线
One Hundred Years of Venus Polarimetry: PICSARR Observations of the Phase Curves
AI总结：
通过PICSARR观测，研究了金星极化特性，发现极地地区存在更高的瑞利散射成分，与以往航天器观测一致。
摘要：
我们报告了关于金星大气散射光极化的高精度观测结果，这些观测是在伯纳德·利奥特开创性研究发表100年后进行的。新的观测包括在不同滤光片范围内的盘积分观测以及成像偏振测量。我们比较了新结果与以往的观测和模型。我们使用现代辐射传输代码重现了1974年汉森和霍文埃的金星极化模型。我们表明新的模型与原模型一致，并使我们能够计算未被原始研究覆盖波长的极化情况，以及在盘面上的极化分布。新的观测结果与过去确定的主要粒子模式大小分布一致。它们与以往研究一致地显示了合相周期之间的相位曲线变化以及短时间尺度上的极化变化，特别是在较高相角（ crescent 阶段）时。成像偏振观测在更红的波长上与模型一致。然而，在紫外波段，极地地区（北纬和南纬约30度范围内）显示出非常不同的极化行为。这一结果的最简单解释是极地地区的瑞利散射成分比赤道和中纬度地区更大，这可能由较低的云顶高度解释，这与以前航天器观测一致。这些紫外极化观测与水平均匀大气模型不一致。
英文摘要：
We report new high-precision observations of the polarization of light scattered from the atmosphere of Venus, made 100 years after the pioneering studies by Bernard Lyot. The new observations include disk-integrated observations in a range of filters as well as imaging polarimetry. We compare the new results with past observations and models. We have reproduced the 1974 modelling of the Venus polarization by Hansen and Hovenier using modern radiative transfer codes. We show that the new models are in good agreement with the originals, and enable us to calculate the polarization for wavelengths not covered by the original study and to model the polarization distribution across the disk. The new observations are in good agreement with past determinations of the size distribution of the predominant particle mode. They agree with past studies in showing variability of the phase curve between synodic cycles and also polarization variability on short timescales, particularly at higher phase angles (crescent phases). Imaging polarimetry observations show good agreement with models for the redder wavelengths. However, observations in the ultraviolet show very different polarization behavior in the polar regions (within about 30 degrees of the north and south poles). The simplest explanation of this result is that there is a larger Rayleigh scattering component in the polar regions than in the equatorial and mid-latitudes and this could be explained by a lower cloud-top height in agreement with previous spacecraft observations. These ultraviolet polarization observations are inconsistent with horizontally homogeneous atmospheric models.
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