AI 中文总结
本研究对比分析火星与月球撞击坑射线、月球冷斑的长度，发现火星射线和月球冷斑长度远超月球反照率射线，二者或通过次级撞击形成，完善了撞击坑射线形成机制的认知。
AI 中文摘要
撞击形成的撞击坑射线在月球上已有充分记录，多数表现为从撞击坑中心径向延伸的高反照率条纹。然而在火星上，撞击坑射线极为罕见，由于其热惯性低于周围地形，仅能通过热成像识别。本研究首次对火星与月球撞击坑射线的长度开展对比分析，涵盖月球反照率射线及冷斑——冷斑是与月球众多最年轻撞击坑相关的射线状热异常。研究结果表明，火星撞击坑射线和月球冷斑的延伸距离均显著大于月球反照率射线，同等直径撞击坑的前者长度是后者的一个数量级。此外，基于热学性质，本研究提出火星撞击坑射线与月球冷斑的形成机制存在关联，通过将热射线整合至现有抛射物模型，完善了对撞击坑射线形成的理解，并指出二者可能通过次级撞击过程具有相似形成机制。深化对这些特征的认知，对行星体的撞击动力学与表面演化研究具有重要意义。
英文摘要
Impact-generated crater rays are well-documented on the Moon, with most appearing as high-albedo streaks extending radially from a crater's center. On Mars, however, crater rays are significantly rarer and discernible only through thermal imaging due to their lower thermal inertia compared to surrounding terrain. This study presents the first comparative analysis between the lengths of Martian and lunar crater rays, including lunar albedo rays and cold spots, which are ray-like thermal anomalies associated with many of the youngest lunar craters. Our findings indicate that both Martian crater rays and lunar cold spots extend significantly farther than lunar albedo rays, with lengths an order of magnitude greater for craters of equivalent diameter. Furthermore, we propose a connection between the formation mechanisms of Martian crater rays and lunar cold spots based on their thermal properties. By integrating thermal rays into existing ejecta models, we refine the understanding of crater-ray formation and suggest that Martian crater rays and lunar cold spots may share a similar formation mechanism via secondary cratering processes. Advancing knowledge of these features has implications for impact dynamics and surface evolution across planetary bodies.
