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Lunar sinuous rilles: Distribution, characteristics, and implications for their origin

机译：月球小溪：分布，特征及其起源

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摘要

Lunar sinuous rilles (SRs) are enigmatic features interpreted to have formed as the result of lava erosion into the lunar surface. While specific SRs have been studied in detail over the past few decades, the most recent general survey of these features was conducted in 1969 using Lunar Orbiter IV and V photographs. The current global study updates the catalog of SRs, using higher resolution SELENE and LRO image and topography data to provide detailed observations and measurements of the rilles observed across the lunar surface. The new survey catalogs more than 200 SRs that vary in length from 2 km to 566 km (median length 33.2 km), in width from 160 m to 4.3 km (median width 480 m), in depth from 4.8 m to 534 m (median depth 49 m), in slope from -1.4° to 0.5° (median slope -0.2°), and in sinuosity index from 1.02 to 2.1 (median sinuosity 1.19). Oceanus Procellarum contains 48% of the rilles mapped in this survey, and these rilles are typically associated with the known centers of volcanism within the Procellarum-KREEP Terrain, the Aristarchus Plateau and the Marius Hills. The current study also constrains the timing of the formation of lunar SRs, using the assumptions that the incised unit represents an upper age limit and the terminal or embaying unit represents a lower age limit. Results indicate that the distribution of ages of rille formation is highly correlated with the emplacement ages of mare units, where the majority of rilles are observed to have formed between 3.0 Ga and 3.8 Ga ago, though some of the features associated with the Aristarchus Plateau may have formed as recently as 1.0 Ga to 1.5 Ga ago. The documented observations can be used to better understand how SRs formed; for example, the range of slopes observed for all rilles (-1.4° to 0.5°) indicates that thermal erosion is likely dominant during the formation of the 78% of rilles that are observed to have formed in solidified mare basalt material, though mechanical erosion is likely to have been a more significant process during the formation of the 25% of observed rilles that originate in the highlands (20% of the mapped rilles crossed from the highlands into the mare), where a thicker regolith is expected to have been more easily eroded.
机译：月球弯曲小溪（SR）是一种神秘的特征，被解释为熔岩侵蚀进入月球表面的结果。在过去的几十年中，对特定的SR进行了详细的研究，但在1969年使用Lunar Orbiter IV和V照片对这些特征进行了最新的综合调查。当前的全球研究使用更高分辨率的SELENE和LRO图像和地形数据更新了SR的目录，以提供对整个月球表面所观察到的小溪的详细观察和测量。新调查对200多个SR进行了分类，其长度从2 km到566 km（中长33.2 km）不等，宽度从160 m到4.3 km（中宽480 m）不等，深度从4.8 m到534 m（中值）不等深度49 m），坡度从-1.4°至0.5°（中度坡度-0.2°），弯曲度指数从1.02至2.1（中度弯曲度1.19）。 Oceanus Procellarum包含本次调查绘制的48％的小溪，这些小溪通常与Procellarum-KREEP地形，阿里斯塔丘斯高原和Marius Hills内的已知火山活动中心有关。当前的研究还假设切开的单位代表年龄上限，而终端或中转单位代表年龄下限，这限制了月球SR形成的时间。结果表明，小形成年龄的分布与母马的进驻年龄高度相关，在这里观察到大多数小have形成于3.0 Ga至3.8 Ga之前，尽管与阿里斯塔丘斯高原有关的某些特征可能形成于1.0 Ga至1.5 Ga之前。记录的观察结果可用于更好地理解SR的形成方式。例如，观察到的所有小溪的斜率范围（-1.4°至0.5°）都表明，在78％的小溪形成过程中，热蚀可能是占主导地位的，而这些小溪是在凝固的母玄武岩材料中形成的，尽管发生了机械腐蚀可能有25％的观察到的小溪起源于高原（在从高地到母马横越的地图小溪中有20％）形成过程中，这是一个更重要的过程，预计较厚的重石块会更多。容易腐蚀。

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