月球熔岩管天窗探测研究进展

汤慧蕾; 胡国平; 陈一平; 张吴明

doi:10.12000/JR25190

月球熔岩管天窗探测研究进展

DOI: 10.12000/JR25190 CSTR: 32380.14.JR25190

中山大学遥感科学与技术学院珠海 519082

基金项目: 广东省珠江人才计划青年拔尖人才(2023QN10H526)，广东省珠江人才计划领军人才(2021CX02S024)

详细信息

作者简介:
汤慧蕾，硕士生，主要研究方向为微波遥感、物理温度模拟

胡国平，博士，副教授，主要研究方向为微波遥感、微波辐射测量建模以及微波数据的反演与处理技术

陈一平，博士，教授，主要研究方向为图像处理、车载(移动)激光雷达数据分析和地理空间人工智能

张吴明，博士，教授，主要研究方向为摄影测量与遥感、激光雷达点云处理及其应用

通讯作者:
胡国平 hugp5@mail.sysu.edu.cn

责任主编：何姿 Corresponding Editor: HE Zi

中图分类号: TP722.6
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出版历程
- 收稿日期: 2025-09-26

Advances in Lunar Lava Tube Skylight Detection

School of Geospatial Engineering and Science, Sun Yat-sen University, Zhuhai 519082, China

Funds: Young Top Talents of Guangdong Pearl River Talent Program (2023QN10H526), Leading Talents of Guangdong Pearl River Talent Program (2021CX02S024)

More Information

Corresponding author: HU Guoping, hugp5@mail.sysu.edu.cn

摘要

摘要: 火山时期由流动熔岩冷却凝固形成的月球熔岩管，因其坚硬外壳能够为管内提供稳定、安全的内部环境，被视为未来月球基地建立的理想地点之一。然而熔岩管埋藏地下数百米至数公里，难以直接探测。目前主要依赖雷达与重力异常探测技术，但轨道雷达探测的分辨率不足以分辨相似形态的地下结构，原位探地雷达存在探测范围有限、易受到近场干扰等问题。重力异常探测则难以精准识别南北走向或亚公里级规模的熔岩管。　　天窗是识别熔岩管的关键标志，可通过光学影像和红外辐射探测热异常进行识别。但光学影像受光照条件制约，难以完整获取天窗的三维几何结构；红外辐射数据受探测深度与分辨率限制(320 m×160 m)，难以捕捉深层热异常及约束坑底物质成分。针对天窗探测方法的技术难点，该文探讨了被动微波探测天窗热异常的可行性，利用其穿透性强、对介电性质敏感的优势，能够深入探测次表层热特征并有效约束坑底物质成分。然而，现有被动微波遥感数据在分辨率(公里级)上难以满足对百米级天窗热异常的精准探测。如何提升微波对百米级天窗的识别能力成为当前技术亟需突破的瓶颈之一。
- 熔岩管探测 /
- 天窗探测 /
- 热异常探测 /
- 被动微波遥感 /
- 月球基地
Abstract: Formed by the cooling and solidification of flowing lava during volcanic activity, lunar lava tubes are considered promising candidates for future lunar bases due to their stable and protective roofs. However, these tubes are typically buried hundreds of meters to kilometers beneath the surface, making direct detection extremely difficult. Current detection methods mainly rely on radar and gravity anomaly analysis. However, the resolution of orbital radar is insufficient to distinguish similar subsurface structures, whereas in situ lunar penetrating radar is limited by a small detection range and vulnerability to near-field interference. Gravity anomaly detection also performs poorly when identifying tubes oriented north–south or with roofs narrower than a kilometer. Skylights serve as critical indicators for locating subsurface tubes and can be identified through optical imagery and infrared radiation thermal anomalies. However, optical images are constrained by illumination conditions, making full three-dimensional reconstruction of skylights difficult. Infrared data are further limited by penetration depth and spatial resolution (320 m × 160 m), which hinders the detection of subsurface thermal anomalies and the assessment of the thermophysical properties of materials at the pit floor. To address these challenges, this paper explores the feasibility of detecting skylight thermal anomalies using microwave radiation. Owing to its penetration capability and sensitivity to dielectric properties, this approach can probe subsurface thermal features and effectively determine the material composition of the pit floor. However, a significant scale disparity exists between the kilometer-scale resolution of current data and the relatively small size of skylights. Therefore, enhancing the detection capability of passive microwave methods for 100-m-scale skylights remains a critical issue that requires immediate attention.
- Lava tube detection /
- Skylight detection /
- Thermal anomaly detection /
- Passive Microwave Remote Sensing /
- Lunar Base

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图 1 熔岩管形成过程示意图^[15]

Figure 1. Schematic diagram of the formation process of a lava tube^[15]

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图 2 熔岩管模式图^[36]

Figure 2. Lava tube pattern diagram^[36]

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图 3 月球熔岩管天窗与月球陨石坑的形态对比图

Figure 3. Morphological comparison between lava tube skylight and lunar crater

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图 4 静海天窗的三维点云侧视图与俯视图

Figure 4. Side view of the full 3D point cloud and nadir view of the Mare Tranquillitatis

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图 5 静海和智海21:00-04:00点(当地太阳时间)通道6与通道8的温度变化平均值差值

Figure 5. The average temperature change difference between Channel 6 and Channel 8 of Mare Tranquillitatis and Mare Ingenii from 9 pm to 4 am (Local Solar Time, LST)

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图 6 具有不同坍塌物质成分的延伸熔岩管与浅洞穴几何模型

Figure 6. Geometric models of extended lava tubes and shallow caves with different collapse materials

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图 7 2D热模型(线)与静海天窗夜间最佳拟合温度(点)

Figure 7. 2D thermal models (lines) compared to Tranquillitatis pit temperatures derived from night-time Diviner Data (points)

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图 8 天窗与背景月壤微波亮度温度差变化图

Figure 8. Microwave brightness temperature difference between skylight and surrounding regolith

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图 9 不同空间分辨率下的天线温度差

Figure 9. Antenna temperature difference under different spatial resolutions

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表 1 部分潜在月球熔岩管参数^[15,25]

Table 1. Basic parameters of some potential lava tubes^[15,25]

地点	纬度	经度	几何参数(m)	深度(m)
马利厄斯丘陵(Marius Hills)	14.2°N	303.3°E	最小宽度：370	-
	13.00°N～15.00°N	301.85°E～304.01°E	-	-
	13.096°N	57.056°W	-	-
	13.603°N	58.047°W	-	-
	14°N	302°E	宽度：400 长度：$ 6\times {10}^{4} $	200～300
	14.3°N	57.5°W	宽度：$ 9\times {10}^{3} $ 长度：$ 6\times {10}^{4} $ 高度：55	605
夏普月溪(Rima Sharp)	35°N～40°N	311°E～316°E	宽度：$ 2\times {10}^{3} $ 长度：$ 7.5\times {10}^{4} $	600
麦兰月溪(Rima Mairan)	36°N	314°E	宽度：$ 3.5\times {10}^{3} $ 长度： $ 1.7\times {10}^{5} $ 高度：550	7500
麦兰-吕姆克(Mairan-Rumker)	41°N	309°W	长度：$ 9\times {10}^{4} $	-
麦兰-吕姆克(Mairan-Rumker)	41°N	306°W	长度：$ 1.8\times {10}^{5} $	-
阿里斯塔克月溪(Rima Aristarchus)	27°N	313°E	宽度：$ 3.75\times {10}^{3} $ 长度：$ 6\times {10}^{4} $ 高度：600	-
施勒特尔延伸(Schröter Extension)	24°N	306°W	长度：$ 6\times {10}^{4} $	-
渥拉斯顿陨石坑(Wollaston D)	35°N	311°W	长度：$ 8\times {10}^{4} $	-
赫歇尔E坑(Hershel E)	33.5°N	324.5°W	长度：$ 2\times {10}^{4} $	-

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表 2 月球部分熔岩管天窗参数^[41]

Table 2. Basic parameters of skylights on the Moon^[41]

名称	纬度	经度	深度(m)	直径(m)
静海(Mare Tranquillitatis)	8.3355°N	33.2220°E	105	100×88
马利厄斯丘陵(Marius Hills)	14.0917°N	303.2299°E	40	55×49
智海(Mare Ingenii)	35.9494°S	166.0559°E	55	104×71
北风暴洋-1(Northern Oceanus Procellarum-1)	35.4097°N	314.3602°E	54	157×108
死湖(Lacus Mortis)	44.9608°N	25.6119°E	60	>165×110
西南丰富海(Southwest Mare Fecunditatis)	6.7521°S	42.7595°E	51	19×15
西南静海(Southwest Mare Tranquillitatis)	4.1438°N	24.6871°E	25	32×26
施吕特陨石坑(Schlüter Crater)	5.8395°S	276.9500°E	57	37×23
高地-1(Highland-1)	43.9662°N	23.0836°E	27	41×37
高地-2(Highland-2)	41.1563°N	18.8206°E	>24	34×27
高地-3(Highland-3)	42.3941°N	320.3076°E	27	45×41

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表 3 探测方法对比表

Table 3. Comparison of Detection Methods

方法	探测方式	原理	优势	局限性
轨道雷达	直接探测	介电常数差异界面产生反射回波	探测范围大	深度分辨率较低；存在多解性
探地雷达	直接探测	介电常数差异界面产生反射回波	高精度探测；局部/小型熔岩管	探测范围有限；易受近场干扰；
重力异常探测	直接探测	质量亏损检测	能探测到深埋于大型熔岩管(公里级) 可估算熔岩管的几何参数	不适用于探测南北走向及小型 (百米级)的熔岩管
光学影像识别	探测天窗间接探测	几何形态特征判别	数据分辨率高；特征直观清晰	受光照条件影响，无法提供完整的天窗内部的形态结构
红外辐射热异常探测	探测天窗间接探测	温度异常识别	突破光照限制；可间接揭示熔岩管的存在	无法甄别坑底热物理特性探测深度有限
被动微波探测	探测天窗间接探测	次表层温度梯度与介电识别	穿透数米月壤次表层；区分天窗坑底物质成分	空间分辨率极低(公里级)

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表 4 典型熔岩管及天窗探测仪器主要参数

Table 4. Main parameters of typical instruments for lava tube and skylight detection

仪器名称	频段/波段	分辨率
月球雷达测深仪 (LRS)	5 MHz	深度分辨率：75 m(真空) 深度分辨率：150 m(经旁瓣压缩)
嫦娥三号/四号测月雷达	低频通道：60 MHz 高频通道：500 MHz	低频通道深度分辨率：米级高频通道深度分辨率：优于0.3 m
重力重建与内部结构实验室(GRAIL)	Ka波段	1200 阶次(4.5 km×4.5 km)
月球勘测轨道器窄角相机 (LRO NAC)	全色(可见光波段)	0.5 m/pixel
红外滤波辐射仪(Diviner)	热红外波段	沿轨道方向320 m 垂直轨道方向160 m (轨道高度50 km)
微波辐射计	3.0, 7.8, 19.35, 37.0 GHz	3 GHz 的空间分辨率约为25 km 其他频率约为17.5 km

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