High‐obliquity excursions on Mars are hypothesized to have redistributed water from the poles to nourish mid‐latitude glaciers. Evidence of this process is provided by different types of viscous flow features (ice‐rich deposits buried beneath sediment mantle) located there today, including lobate debris aprons (LDAs). During high‐obliquity extremes, ice may have persisted even nearer the equator, as indicated by numerous enigmatic depressions bounded on one side by either isolated mesas or scarps, and on the other by a lava unit. These depressions demarcate the past interaction between flowing lava and ghost LDAs (GLDAs), which have long since disappeared. We term these features GLDA depressions, about which little is known besides their spatial extent. This collection of depressions implies tropical ice loss over an area ∼100,000 km². To constrain their history in Kasei Valles, we derive model ages for GLDA depressions, mesas, and the lava flow from crater counts. We use a 2D model of glacial ice constrained by the topography of GLDA depressions to approximate the surface and volume of former glacial ice deposits. The model reconstructs former ice surfaces along multiple flow lines orientated normal to GLDA depression boundaries. This reconstruction indicates that 1,400–3,500 km³ of ice—similar to that present in Iceland on Earth—existed at ∼1.3 Ga when the lava was emplaced. Dating shows that the GLDAs survived for up to ∼1 billion years following lava emplacement, before its final demise.

中文翻译：

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火星Kasei Valles的晚期亚马逊冰生存

据推测，火星上的高倾角游览是将两极的水重新分配给了中纬度冰川。今天存在于此处的各种类型的粘性流动特征（富含冰的沉积物沉积在沉积物幔下面）提供了这一过程的证据，包括叶状碎片围裙（LDA）。在高倾角的极端情况下，冰可能甚至在赤道附近仍然存在，这表现为无数的凹陷，其一侧被孤立的台地或陡坡界定，而另一侧则被熔岩单元界定。这些洼地划定了流动的熔岩和幽灵LDA（GLDA）之间的过去相互作用，而这些相互作用早就消失了。我们称这些特征为GLDA凹陷，除了其空间范围外，对此知之甚少。这些洼地的集合意味着热带冰在约100,000公里的范围内流失²。为了限制它们在Kasei Valles的历史，我们从火山口计数中得出GLDA凹陷，台地和熔岩流的模型年龄。我们使用受GLDA凹陷地形约束的冰川冰的2D模型来估算以前冰川冰沉积物的表面和体积。该模型沿多条垂直于GLDA凹陷边界的流线重建了以前的冰面。重建结果表明，放置熔岩时，在约1.3 Ga处存在1,400–3,500 km ³的冰，类似于地球上冰岛的冰。约会表明，GLDAs在熔岩沉积后存活了大约10亿年，直到最终消失。