月球静海环形凹陷穹丘的微波雷达散射特征分析

高强山; 张锋; 党亚南; 梁莉婷; 牛胜利; 殷浩林; 苏子昂

doi:10.12000/JR25193

月球静海环形凹陷穹丘的微波雷达散射特征分析

DOI: 10.12000/JR25193 CSTR: 32380.14.JR25193

高强山¹,
张锋^1, ,,
党亚南²,
梁莉婷¹,
牛胜利¹,
殷浩林^{1, 3},
苏子昂^{1, 3}

1.
中国科学院国家空间科学中心北京 100190
2.
中国科学院空天信息创新研究院北京 100190
3.
中国科学院大学北京 100049

基金项目: 国家自然科学基金(62495034, 12273044, 12303065)

详细信息

作者简介:
高强山，博士，主要研究方向为雷达图像处理，建模及地质过程解译

张　锋，研究员，主要研究方向为类地行星表面特征、成因及相关地质过程研究，尤其火山地质学

党亚南，助理研究员，主要研究方向为行星表面水文地貌特征及其成因、月球火山地貌的SAR特征分析等

梁莉婷，副研究员，主要研究方向为极化分解理论、极化散射建模及SAR遥感应用

牛胜利，博士，主要研究方向为行星遥感与地质学

殷浩林，博士，主要研究方向为行星遥感与地球物理

苏子昂，硕士，主要研究方向为月球火山地貌的形貌特征与演化分析

通讯作者:
张锋 zhangfeng@nssc.ac.cn

责任主编：陆萍萍 Corresponding Editor: LU Pingping

中图分类号: P184
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出版历程
- 收稿日期: 2025-09-29

Microwave Radar Scattering Characteristics of Ring-Moat Dome Structures in Mare Tranquillitatis on the Moon

1.
National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
2.
Aerospace Information Research Institute, Chinese Academy of Sciences, Beijing 100190, China
3.
University of Chinese Academy of Sciences, Beijing 100049, China

Funds: The National Natural Science Foundation of China (62495034, 12273044, 12303065)

More Information

Corresponding author: ZHANG Feng, zhangfeng@nssc.ac.cn

摘要

摘要: 环形凹陷穹丘(RMDS)是发育于月海玄武岩表面的一类小型穹隆构造。其平均高度仅3～4 m，直径约200 m，形态低缓；因其数量巨大，已成为理解月球火山活动与岩浆热力学行为的重要研究对象。尽管光学遥感观测结果支持RMDSs的火山作用成因机制，但仍有学者提出了其他可能性。因此，其成因的确证仍需更多地质证据的支撑。微波雷达因其穿透性而具备探测月面次表层结构与物理特性的独特优势，然而截至目前，针对RMDSs微波雷达散射特征的研究仍处于空白。该文重点利用星载雷达微型射频仪(Mini-RF)和地基雷达阿雷西博(Arecibo)的S波段(波长12.6 cm)数据，以静海盆地月海表面一RMDSs密集分布区为研究区，开展其雷达后向散射功率和圆极化率(CPR)等特征分析。结果显示：(1) RMDSs以低后向散射功率为基本特征，这与泡沫岩浆成因理论预测的雷达弱散射特征高度吻合。该理论认为，RMDSs表面约2～3 m深度范围内覆盖的亚毫米级细粒物质，是导致其呈现低强度雷达散射回波的主要原因；(2)受撞击作用、地形起伏及物质坡移等因素的影响，部分RMDSs局部区域表现出不同程度的后向散射增强特征，但长期风化会弱化这一特征；(3) RMDSs的雷达散射系数及CPR均值统计结果均与火山碎屑堆积物高度接近，这表明二者的表面物理性质相似，其表面物质颗粒尺度应与以微米至毫米级细颗粒为主的火山碎屑物相当。上述研究进一步证实，多波段、高分辨率、多极化雷达数据能够为RMDSs的精细化研究提供更丰富的地质证据。这不仅深化了对RMDSs形成与演化机制的认识，同时也为后续月表火山地貌的微波遥感探测研究提供了有价值的参考。
- 环形凹陷穹丘 /
- 微波雷达 /
- 月海玄武岩 /
- 火山作用 /
- 月球
Abstract: The ring-moat dome structure (RMDS) is a small-scale domical landform that develops on the lunar mare basalt surface. With an average height of only 3–4 m and a mean diameter of approximately 200 m, these features display a low-relief morphology. Owing to their abundance, RMDSs have become an important subject for understanding lunar volcanic activity and magmatic thermodynamic processes. Although optical remote sensing observations support a volcanic origin for RMDSs, alternative hypotheses have been proposed. Therefore, confirming their genesis requires further geological evidence. Microwave radar provides a distinct advantage in probing the subsurface structure and physical properties of the Moon owing to its penetrative capability. However, to date, no studies have examined the microwave radar scattering characteristics of RMDSs. This paper therefore analyzes the radar backscatter power and circular polarization ratio (CPR) characteristics of RMDSs using S-band (12.6 cm wavelength) data acquired by the spaceborne Miniature Radio Frequency (Mini-RF) instrument and the ground-based Arecibo radar. The study area is a region densely populated with RMDSs on the mare surface within the Mare Tranquillitatis basin. The results indicate the following: 1) RMDSs exhibit low backscatter power, which is highly consistent with the weak radar scattering predicted by the foamy magma genetic model. According to this model, the primary cause of the low-intensity radar echo is the presence of submillimeter-scale fine-grained materials within the uppermost ～2–3 m depth range. 2) Influenced by impact cratering, topographic variations, and mass wasting, some RMDSs display localized enhancement of backscatter to varying degrees; however, prolonged space weathering diminishes this effect. 3) The mean statistical values of the radar backscatter coefficient and the CPR for RMDSs are remarkably close to those of pyroclastic deposits, indicating that their surface physical properties are analogous and that the particle size of their surface materials should be comparable to those of pyroclastic materials, which are predominantly fine-grained particles in the micrometer-to-millimeter range. These findings further confirm that multiband, high-resolution, and multipolarization radar data can yield richer geological evidence for the detailed investigation of RMDSs. This not only deepens the understanding of RMDS formation and evolutionary mechanisms but also provides a valuable reference for future microwave remote sensing exploration of lunar volcanic landforms.
- Ring Moat Dome Structure (RMDS) /
- Microwave radar /
- Mare basalt /
- Volcanism /
- The Moon

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图 1 研究区(红色矩形框)位置

Figure 1. Location of the study area (red rectangular box)

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图 2 研究区雷达图像(底图为Kaguya TC evening map)

Figure 2. Radar images of the study area (The base map is the Kaguya TC evening map)

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图 3 一撞击坑溅射物范围内的RMDSs

Figure 3. RMDSs located within the ejecta deposit of an impact crater

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图 4 与撞击坑部分重叠的RMDSs

Figure 4. RMDSs partially overlapping an impact crater

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图 5 表面有小型撞击坑的RMDSs

Figure 5. RMDSs with small impact craters on the surface

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图 6 静海CPR值统计分析区域划分与区域c地区的RMDSs分布图

Figure 6. Statistical zoning of CPR values in Mare Tranquillitatis and distribution of RMDSs in Region C

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图 7 RMDSs及其所在月海CPR值的统计直方图

Figure 7. Statistical histograms of CPR values of RMDSs and their host mare

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图 8 RMDSs、不规则月海斑块Ina及火山碎屑堆积物的OC散射系数与CPR值散点图

Figure 8. Scatter plots of RMDSs, irregular mare patch Ina, and pyroclastic deposits in terms of OC scattering coefficient and CPR values

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图 9 非撞击因素引起RMDSs局部出现较高雷达散射强度的案例

Figure 9. Cases of locally elevated radar scattering intensity of RMDSs caused by non-impact factors

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图 10 串珠状(或链状)RMDSs的雷达信号散射特征

Figure 10. Radar scattering characteristics of beaded (or chain) RMDSs

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表 1 RMDSs与其他火山地貌的雷达散射特征均值统计表

Table 1. Statistical results of mean radar scattering characteristics for RMDSs and other volcanic landforms

特征描述	OC散射系数(dB)	CPR值	样本数
撞击坑溅射物覆盖的RMDSs	–13.70±1.64	0.47±0.23	256
	–12.52±1.54	0.56±0.26	172
	–11.64±1.65	0.59±0.28	118
	–13.93±2.01	0.45±0.23	1063
	–10.81±1.68	0.52±0.30	188
	–10.44±1.49	0.52±0.25	150
与撞击坑叠置的RMDSs	–13.74±2.40	0.52±0.21	771
与撞击坑叠置的RMDSs	–14.67±2.01	0.49±0.25	96
表面有亮色小坑的RMDSs	–16.46±1.70	0.34±0.18	4711
表面有亮色小坑的RMDSs	–16.31±1.89	0.35±0.19	2486
无撞击作用影响的RMDSs	–16.95±1.75	0.37±0.24	155
无撞击作用影响的RMDSs	–16.58±1.71	0.32±0.17	171
火山碎屑堆积物	–15.71±1.20	0.31±0.08	/
火山碎屑堆积物	–16.85±1.30	0.33±0.08	/
Ina月海斑块内石块单元	–10.55±3.76	0.40±0.19	/
月海斑块内退化撞击坑溅射物	–12.20±1.45	0.49±0.09	/
月海斑块内退化撞击坑溅射物	–12.52±1.99	0.49±0.14	/

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