Geological and evolutionary characteristics of the Gagarin Region on the far side of the Moon
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摘要: 以月球背面加加林地区为研究对象，采用多源遥感数据解译，通过地质要素定量统计、分布特征与成因分析等研究方法，揭示了月球背面典型区域的地质特征，进而探讨了加加林地区区域地质演化历史，初步建立了该区地质特征与月球演化过程之间的联系。 研究结果表明：区内发育的全月最长深部断裂的形成为南极艾肯撞击事件与月球热膨胀等内外应力共同作用的结果；自南极−艾肯盆地向外延伸的多处月壳厚度的线性异常延伸至月球正面各大盆地，说明在月球深部，月球背面南极−艾肯盆地的影响范围可以辐射到月球正面单元；月球背面加加林地区撞击坑数量与面积的变化规律与月球所处的地月系及太阳系演化进程有关；撞击坑定量统计结果及玄武岩单元定年结果表明，艾肯纪至雨海纪是加加林地区外动力地质作用的活跃时期，雨海纪是其内动力地质作用的活跃时期。Abstract:
Objective This study focuses on the Gagarin region on the far side of the Moon, aiming to reveal the geological characteristics, distribution features, and genesis of typical areas on the lunar far side. Additionally, it seeks to explore the regional geological evolution history of the Gagarin region. Methods The study primarily employs methods such as multi-source remote sensing data interpretation, regional geological mapping, and quantitative analysis of geological elements' quantity and distribution characteristics. Results (1) 656 impact craters were discovered in the study area, of which 552 have diameters greater than 20 kilometers. Approximately 71.5% of the Gagarin region is covered by ancient basins and their ejecta from the Aitken period. Based on comprehensive area and diameter data, the Aitken period is identified as the geological era with the largest proportion of large impact craters (diameter greater than 70 kilometers) and the largest average diameter. From the Aitken period to the Copernican period, the total area of impact craters in each geological era shows a decreasing trend from old to new. (2) In the study area, six parallel lunar grabens, 62 lobate scarps, one sinuous rille , 50 crater floor fractures, and 70 shallow faults were discovered. It also includes parts of the two longest inferred deep faults on the Moon, originating from the South Pole–Aitken tectonic zone and almost spanning the entire highland tectonic zone. According to Bouguer gravity anomalies and crustal thickness data, linear crustal thickness anomalies extending outward from the South Pole–Aitken basin reach the major basins on the near side of the Moon. (3) The Gagarin region is primarily located in the anorthositic highlands on the far side of the Moon. The rocks mainly consist of ferroan anorthosite (fa) suites, with some crater floors showing magnesium anorthosite (ma) suites. In the central and southern parts of the Gagarin region, low-titanium (TiO2 > 1.5 and < 4.5) and very low-titanium (TiO2 < 1.5) basalts are sparsely distributed on the floors of certain impact craters and basins. (4) For this study, we selected impact craters such as Aitken and Van der Graaf, with diameters ranging from 350 to 1400 m, for dating analysis. The results of crater size-frequency distribution dating indicate ages of 3.47 GA and 3.32 GA, respectively. (5) The quantitative statistics of impact craters and the dating results of basalt units indicate that the Aitkenian to Imbrian periods were active periods of external dynamic geological processes in the Gagarin region, while the Imbrian period was an active period of internal dynamic geological processes. Conclusion (1) The region’s longest and deepest faults are the result of the combined effects of the South Pole–Aitken impact event and internal and external stresses, including lunar thermal expansion. (2) The variations in the number and size of impact craters in the Gagarin region on the far side of the Moon are related to the evolution of the Earth–Moon system and the solar system. (3) Based on the quantitative statistical results of impact craters and the dating results of basalt units, this study elucidates the regional geological evolution history, and different stages of the geological processes in the Gagarin region were divided according to the active periods and stage characteristics of internal and external dynamic geological processes. Significance The study revealed the geological features of key areas on the far side of the moon, delving into the geological history of the Gagarin region and tentatively establishing a correlation between its geological traits and the lunar evolutionary history. -
Key words:
- Lunar geology /
- Gagarin Basin /
- multi-source remote sensing data /
- geological evolution
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图 1 1∶250万月球地质图分幅及加加林地区位置示意图（底图为CE-1 CCD影像数据，分辨率为120 m；数据来源月球与行星数据发布系统
https://moon.bao.ac.cn/ ；图中经纬度注记中无负号代表东经经度和北纬纬度，有负号为西经经度和南纬纬度，如−30°代指南纬30°，150°代表东经150°，下同）Figure 1. The map sheet of the 1∶2500000 geological map of the moon and the position of the Gagarin region (Base map is CE-1 CCD image data, with a resolution of 120 m; data source: Moon and Planetary Data System https://moon.bao.ac.cn/; In the latitude and longitude annotation in the figure, no negative sign represents north latitude, and a negative sign represents south latitude, such as –30° indicating 30° south latitude, the same below.)
图 2 加加林地区地貌示意图（底图为LOLA高程数据；数据来源NASA官网
https://disc.gsfc.nasa.gov/ ）Figure 2. Topographic schematic map of the Gagarin region (Base map is LOLA elevation data; data source: NASA official webbsite
https://disc.gsfc.nasa.gov/ )
图 4 月球地质年代划分方案（据郭弟均等，2014；凌宗成等，2014修改）
Figure 4. Geologic chronology of the moon (modified after Guo et al., 2014; Ling et al., 2014 )
图 7 加加林地区月堑、叶状陡坎解译结果
a—部分月堑分布位置（底图为 WAC 影像，其中AA′为月堑剖面线，箭头指示月堑位置）；b—对应区域高程图（底图为 LOLA 数据和 WAC影像数据叠加，箭头指示月堑位置）；c—AA′剖面线对应地形剖面；d—部分叶状陡坎分布位置（底图为WAC 影像，其中BB′为叶状陡坎剖面线，箭头指示叶状陡坎位置）；e—叶状陡坎分布区域高程图（底图为 LOLA 数据和 WAC影像数据叠加，箭头指示叶状陡坎位置）；f—BB′剖面线对应地形剖面
Figure 7. Interpretation results of lunar grabens and lobate scarps in the Gagarin region
(a) Partial distribution map of lunar grabens (Base map is WAC image, where AA′ represents the section line of lunar grabens, with arrows indicating the position of lunar grabens); (b) Elevation map of the corresponding region (Base map is superimposed by LOLA data and WAC image data); (c) Topographic section corresponding to the section line AA′; (d) Partial distribution map of lobate scarps (Base map is WAC image, where BB′ represents the section line of lobate scarps, with arrows indicating the position of lobate scarps); (e) Elevation map of the lobate scarp distribution area (Base map is superimposed by LOLA data and WAC image data, with arrows indicating the position of lobate scarps); (f) Topographic section corresponding to the section line BB′
图 8 加加林地区月溪、坑底断裂解译结果
a—研究区内部分月溪分布位置（底图为 WAC 影像，其中CC'为月溪剖面线，箭头指示月溪位置）；b—对应区域高程图（底图为 LOLA 数据和 WAC影像数据叠加）；c—CC'剖面线对应地形剖面；d—部分坑底断裂分布位置（底图为 WAC 影像，其中DD'为坑底断裂剖面线）；e—坑底断裂分布区域高程图（底图为 LOLA 数据和 WAC影像数据叠加）；f—DD'剖面线对应地形剖面
Figure 8. Interpretation results of sinuous rilles and crater-floor fractures in the Gagarin map
(a) Partial distribution map of the sinuous rille (Base map is WAC image, where CC′ represents the section line of the sinuous rille, with arrows indicating the position of the sinuous rille); (b) Elevation map of the corresponding region (Base map is superimposed by LOLA data and WAC image data); (c) Topographic section corresponding to the section line CC'; (d) Partial distribution map of crater-floor fractures (Base map is WAC image, where DD′ represents the section line of crater-floor fractures); (e) Elevation map of the crater-floor fracture distribution area (Base map is superimposed by LOLA data and WAC image data); (f) Topographic section corresponding to the section line DD'
图 9 南极−艾肯盆地及邻区布格重力异常与月壳厚度（布格重力数据来自 GRAIL任务发布的 1200 阶布格异常模型，Goossens et al.，2020；月壳厚度数据使用GL0420A重力场模型计算得到，Wieczorek et al.，2013）
Figure 9. Bouguer gravity anomaly and lunar shell thickness of the South Pole–Aiken Basin and adjacent areas (The Bouguer gravity data is derived from the 1200-order Bouguer anomaly model published by the GRAIL mission from Goossens et al., 2020; The lunar shell thickness data are derived from the lunar shell thickness model calculated by Wieczorek et al. using GL0420A gravitational field model. Data source: Wieczorek et al., 2013)
图 10 月球推测深部断裂识别结果及主要撞击盆地位置
a、b为全月最长的2条推测深部断裂的组成部分
Figure 10. Recognition results of inferred deep faults and location of main impact basins on the Moon
a and b are the components of the two longest inferred deep faults on the moon.
图 11 不同地质年代各直径范围不同撞击坑占比
Figure 11. The proportion of impact craters of different diameters in different geological ages
图 12 不同地质年代坑物质面积与数量占比
Figure 12. The proportion of crater material area and quantity in different geological ages
图 13 加加林地区各时期外动力地质作用
图例说明同图5a—艾肯纪撞击坑（盆地）；b—酒海纪撞击坑（盆地）；c—雨海纪撞击坑（盆地）；d—爱拉托逊纪−哥白尼纪撞击坑
Figure 13. Impact craters (basins) formed in different periods by exodynamic geological processes in the Gagarin region
(a) Aitkenian Period; (b) Nectarian Period; (c) Imbrian Period; (d) Eratosthenian Period–Copernican PeriodRefer to Fig.5 for legend details.
表 1 研究区撞击坑直径和数量
Table 1. Craters' diameters and numbers in the study area
直径/km 不同地质年代撞击坑的数量/个 艾肯纪 酒海纪 雨海纪 爱拉托逊纪 哥白尼纪 年代未确定 总计 <15 14 33 95 12 7 53 214 <35 39 51 60 16 1 36 203 <70 43 25 14 4 0 0 86 >70且<200 31 13 5 0 0 0 49 总计 127 122 174 32 8 89 552 
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