地球信息科学学报 ›› 2012, Vol. 14 ›› Issue (5): 618-626.doi: 10.3724/SP.J.1047.2012.00618

• 陆地表层系统模拟与分析 • 上一篇    下一篇

月球正面撞击坑的空间分布特征分析

周增坡1,2, 程维明1*, 万丛1,2, 侯琳1,3   

  1. 1. 中国科学院地理科学与资源研究所 资源与环境信息系统国家重点实验室,北京 100101;
    2. 中国科学院大学,北京 100049;
    3. 东北师范大学城市与环境科学学院,长春 130024
  • 收稿日期:2012-05-08 修回日期:2012-08-13 出版日期:2012-10-25 发布日期:2012-10-25
  • 通讯作者: 程维明(1973-),男,博士,副研究员,研究方向为地貌、制图及遥感与GIS技术应用。 E-mail:chengwm@lreis.ac.cn E-mail:chengwm@lreis.ac.cn
  • 作者简介:周增坡(1982-),男,河南南阳人,博士研究生,研究方向为月貌及GIS应用。E-mail:zhouzp@lreis.ac.cn
  • 基金资助:

    国家自然科学基金项目(41171332);中国科学院地理科学与资源研究所知识创新项目(201001005)。

Analysis on the Spatial Distribution Characteristics of Lunar Near Side Impact Craters

ZHOU Zengpo1,2, CHENG Weiming1*, WAN Cong1,2, HOU Lin1,3   

  1. 1. State Key Laboratory of Resources and Environmental Information Systems, Institute of Geographic Sciences and Natural Resources Research, CAS, Beijing 100101, China;
    2. University of Chinese Academy of Sciences, Beijing 10049, China;
    3. The School of Urban and Environmental Science, Northeast Normal University, Changchun 130024, China
  • Received:2012-05-08 Revised:2012-08-13 Online:2012-10-25 Published:2012-10-25

摘要: 通过IAU最新公布的撞击坑名录、"嫦娥一号"影像与DEM数据,本文使用数理统计和空间分析的方法研究了月球正面撞击坑分布的空间不均衡性。主要体现在:(1)月球正面直径较大的撞击坑主要分布在月陆区域,且集中趋势明显,而月海区域直径较大的撞击坑分布较少,周围有大量直径较小的撞击坑;(2)直径较大的撞击坑在月表具有一定随机性,而直径较小的撞击坑在月表的集中性明显; (3)赤道区域的撞击坑密度小于两极区域,前导半球的撞击坑数量小于后随半球;月海区域的撞击坑密度小于月陆区域;密度最大的区域位于月球正面的中南部;(4)月球正面深度大于2.5km的撞击坑主要集中在月陆区域,且在南极的中央经线附近更为集中;在57°N至24°S之间,深径比处于较高水平,最大值出现在14°N附近,均值在0.14左右波动,自该区域至南北两极,深径比逐渐减小,并在南极附近出现最小值;(5)月陆区域撞击坑坡度最大值的均值大于月海区域;坡度最大值的均值规律性明显,即自赤道至两极,撞击坑坡度最大值的均值逐渐增大。月球撞击坑的空间分布具有一定空间集聚性、经向和纬向差异性,该特征与撞击坑形成理论间的耦合关系仍需深入研究。

关键词: 月球正面, 不均衡性, 撞击坑, 嫦娥一号

Abstract: The mathematical statistics and spatial analyses for lunar near side impact craters are used to unravel potential spatial heterogeneity based on the crater nomenclature released by International Astronomical Union (IAU) and topography and imagery data from Chang'E-1(CE-1).The spatial heterogeneity is mainly embodied in the following aspects: (1)the craters with larger diameters dominantly distribute in the highland and show obvious concentration tendency, however, the mare have much fewer larger craters, accompanying by munificent smaller craters; (2) larger craters have the characteristics of randomness and the smaller crater are concentrated in local areas; (3) density differences: the regions closer to equator have higher crater frequencies than the regions to the pole; the trailing hemisphere is cratered at a higher rate than the leading hemisphere; the most densely cratered region is located in the south-central part of the lunar nearside; (4) depth-diameter ratios differences: the craters with depth larger than 2.5 km almost are found in the highland, and there is a marked concentration of points around the central meridian where it cuts through the southern continent; between 57°N and 24°S, the ratio is at a high level; the maximum value occurs near 14°N, and the average value fluctuates at 0.14; approaching the poles, the ratios are becoming smaller, and the minimum value occurs at the south pole region; and (5) gradient differences: the average of crater's maximum gradient in highland is far greater than the value of craters in mare; the average of crater's maximum gradient shows apparent pattern: from lunar equator to the poles, the average of crater maximum gradient increases gradually. The spatial pattern of lunar craters shows marked regional differentiation characteristics, and the relationship between the pattern and the crater forming theory remains much work to be done before the ultimate goal can be reached.

Key words: lunar near side, asymmetry, impact craters, Chang'E-1(CE-1)