The Thickness and Volume of Young Basalts Within Mare Imbrium
Chen, Yuan; Li, Chunlai; Ren, Xin; Liu, Jianjun; Wu, Yunzhao; Lu, Yu; Cai, Wei; Zhang, Xunyu
2018
发表期刊JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
卷号123期号:2页码:630-645
摘要Basaltic volcanism is one of the most important geologic processes of the Moon. Research on the thickness and volume of late-stage basalts of Mare Imbrium helps better understand the source of lunar volcanism and eruption styles. Based on whether apparent flow fronts exist or not, the late-stage basalts within Mare Imbrium were divided into two groups, namely, Upper Eratosthenian basalts (UEm) and Lower Eratosthenian basalts (LEm). Employing the topographic profile analysis method for UEm and the crater excavation technique for LEm, we studied the thickness and distribution of Eratosthenian basalts in Mare Imbrium. For the UEm units, their thicknesses were estimated to be similar to 16-34 (2)m with several layers of individual lava (similar to 8-13m) inside. The estimated thickness of LEm units was similar to 14-45(1)m, with a trend of reducing thickness from north to south. The measured thickness of late-stage basalts around the Chang'E-3 landing site (similar to 371m) was quite close to the results acquired by the lunar penetrating radar carried on board the Yutu Rover (similar to 35m). The total volume of the late-stage basalts in Mare Imbrium was calculated to be similar to 8,671 (320)km(3), which is 4 times lower than that of Schaber's estimation (similar to 4x10(4)km(3)). Our results indicate that the actual volume is much lower than previous estimates of the final stage of the late basaltic eruption of Mare Imbrium. Together, the area flux and transport distance of the lava flows gradually decreased with time. These results suggest that late-stage volcanic evolution of the Moon might be revised.Plain Language Summary The late stage younger than 3.1Ga volcanism of the Moon deposited large areas of basalts in Mare Imbrium and Oceanus Procellarum. These basalts have different colors (dark and blue) compared to old basalts sampled by Apollo and Luna missions. In order to understand how these young basalts erupted in Mare Imbrium, we estimated their thickness and volume using multiple data. Using detailed visible and near-infrared spectral data in combination with topographic information, we estimated the height of lava flows and the thickness of late-stage rocks excavated by impact craters. Our results indicate that these young basalts have a thickness of tens of meters and a total volume of similar to 8,671 (+/- 320)km(3). Both values are smaller than those of previous estimates, suggesting a smaller volcanic activity than previously thought. These results indicate that the magmatic activity gradually weakened in this region.
语种英语
WOS记录号WOS:000427479000017
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被引频次:1[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://libir.pmo.ac.cn/handle/332002/18077
专题近地天体探测和太阳系天体研究团组
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Chen, Yuan,Li, Chunlai,Ren, Xin,et al. The Thickness and Volume of Young Basalts Within Mare Imbrium[J]. JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS,2018,123(2):630-645.
APA Chen, Yuan.,Li, Chunlai.,Ren, Xin.,Liu, Jianjun.,Wu, Yunzhao.,...&Zhang, Xunyu.(2018).The Thickness and Volume of Young Basalts Within Mare Imbrium.JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS,123(2),630-645.
MLA Chen, Yuan,et al."The Thickness and Volume of Young Basalts Within Mare Imbrium".JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS 123.2(2018):630-645.
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