来自蒸发岩分布的土卫六气候历史证据
Evidence of Titan's Climate History from Evaporite Distribution
摘要：
土星卫星泰坦上的水冰贫乏，亮度为5- $μ$ m的物质先前被地貌学确定为钾长石。在这里，我们提出了一个全球分布的发生5- $μ$ m-明亮的光谱单位，确定与卡西尼号的可见光红外测绘光谱仪（VIMS）和雷达检查时，可能的。我们探讨的可能性，这些事件是蒸发矿床。5- $μ$ m-明亮物质覆盖泰坦表面的1%，并且不限于两极（唯一具有广泛、长寿的表面液体的区域）。我们发现最大的面积集中在赤道盆地Tui Regio和Hotei Regio。我们的解释，5- $μ$ m-明亮的材料和湖床之间的相关性的基础上，意味着有足够的液体存在于某个时候，以创建所观察到的5- $μ$ m-明亮的材料。我们解决气候的影响，周围缺乏蒸发岩材料在南极盆地：如果南极盆地在过去的某个时候被填充，那么蒸发岩在哪里？
英文摘要：
Water-ice-poor, 5-$μ$m-bright material on Saturn's moon Titan has previously been geomorphologically identified as evaporitic. Here we present a global distribution of the occurrences of the 5-$μ$m-bright spectral unit, identified with Cassini's Visual Infrared Mapping Spectrometer (VIMS) and examined with RADAR when possible. We explore the possibility that each of these occurrences are evaporite deposits. The 5-$μ$m-bright material covers 1\% of Titan's surface and is not limited to the poles (the only regions with extensive, long-lived surface liquid). We find the greatest areal concentration to be in the equatorial basins Tui Regio and Hotei Regio. Our interpretations, based on the correlation between 5-$μ$m-bright material and lakebeds, imply that there was enough liquid present at some time to create the observed 5-$μ$m-bright material. We address the climate implications surrounding a lack of evaporitic material at the south polar basins: if the south pole basins were filled at some point in the past, then where is the evaporite?
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