论文标题
从云层上方的近红外成像金星的表面：有效空间分辨率的新分析理论
Imaging Venus' Surface at Night in the Near-IR From Above Its Clouds: New Analytical Theory for the Effective Spatial Resolution
论文作者
论文摘要
近红外有少数光谱窗，我们可以看到地球夜晚的金星表面。因此，我们姐妹星球的表面是通过金星孔平台上的传感器（Venus Express，Akatsuki）和其他行星（伽利略，卡西尼）飞行的。到目前为止，最诱人的发现是可能活动火山的暗示。然而，金星的灼热（c。475摄氏度）发出的热辐射必须穿过50至70 km高度之间的不透明云以及亚云的气氛。在云层中，光线不是被吸收的，而是散落的，很多时候。这会使表面图像模糊到最小可辨别的特征大约100 km，全宽的半程最大最大（FWHM），并且已经使用数值模型来解释这一点。我们描述了一个新的分析建模框架，用于预测大气点传播函数（APSF）的宽度，这是决定从空间中表面成像的有效分辨率的原因。我们对1到1.2微米光谱范围的APSF宽度的最佳估计值约为130 km fWHM。有趣的是，这比约100 km的公认值大一些，该值基于视觉图像检查和数值模拟。
There are a handful of spectral windows in the near-IR through which we can see down to Venus' surface on the night side of the planet. The surface of our sister planet has thus been imaged by sensors on Venus-orbiting platforms (Venus Express, Akatsuki) and during fly-by with missions to other planets (Galileo, Cassini). The most tantalizing finding, so far, is the hint of possible active volcanism. However, the thermal radiation emitted by the searing (c. 475 degrees C) surface of Venus has to get through the opaque clouds between 50 and 70 km altitude, as well as the sub-cloud atmosphere. In the clouds, the light is not absorbed but scattered, many times. This results in blurring the surface imagery to the point where the smallest discernible feature is roughly 100 km in size, full-width half-max (FWHM), and this has been explained using numerical models. We describe a new analytical modeling framework for predicting the width of the atmospheric point-spread function (APSF), which is what determines the effective resolution of surface imaging from space. Our best estimates of the APSF width for the 1-to-1.2 micron spectral range are clustered around 130 km FWHM. Interestingly, this is somewhat larger than the accepted value of about 100 km, which is based on visual image inspection and numerical simulations.
