The transition from complex crater to peak-ring basin on the Moon: New observations from the Lunar Orbiter Laser Altimeter (LOLA) instrument
The transition from complex crater to peak-ring basin on the Moon: New observations from the Lunar Orbiter Laser Altimeter (LOLA) instrument
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DOI：
10.1016/j.icarus.2011.05.030
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发表时间：
2011-08-01
期刊：
影响因子：
3.2
通讯作者：
Neumann, Gregory A.
中科院分区：
文献类型：
--
作者：
Baker, David M. H.;Head, James W.;Neumann, Gregory A.
行星天体上的撞击坑随着大小的增加，从简单到复杂，再到峰环盆地，最后到多环盆地。对具有中心峰的复杂陨石坑和多环盆地之间关系的重要理解是分析原盆地（表现出一个边缘峰和一个内环加上一个中心峰）和峰环盆地（表现出一个边缘峰和一个内环）。新的数据可以改进对月球上这些过渡特征的描绘和分类。我们利用月球勘测轨道器上的月球轨道激光高度计（LOLA）提供的128像素/度网格化地形数据，结合图像拼接，对月球上直径为100 ~ 50 km的陨石坑进行了调查，并更新了现有的月球峰环盆地和原盆地目录。我们更新的目录包括17个峰环盆地（环顶直径为207 ~ 582 km，几何平均为343 km）和3个原盆地（137 ~ 170 km，几何平均为157 km）。先前研究推断为多环盆地的几个盆地（Apollo, Moscoviense, Grimaldi, Freundlich-Sharonov， Coulomb-Sarton和Korolev）现在被归类为峰环盆地，因为它们与月球峰环盆地形态相似，并且没有确定的超过两个的地形环结构。我们还在我们的目录中包括23个陨石坑，它们表现出小的环状簇状山峰（50-205公里，几何平均= 81公里）；一个（洪堡）展示了一个边缘-波峰直径和内部形态，可能是形成峰环过程的独特过渡。对月球上峰环盆地的环直径（D-ring）和环顶直径（D-r）的幂律拟合[D-ring = 0.14 +/- 0.10(D-r)(1.21 +/- 0.13)]揭示了一种与水星上峰环盆地直径的幂律拟合[D-ring = 0.25 +/- 0.14(D-rim)(1.13 +/- 0.10)]非常相似的趋势[Baker， D.M.H.等人[2011]。星球。空间科学。[印刷]。月球上峰环盆地和原盆地的环/边缘-波峰比与边缘-波峰直径的关系图也揭示了一个连续的、非线性的趋势，类似于在水星和金星上观察到的趋势，表明原盆地和峰环盆地是盆地形态连续体的一部分。月球上峰环盆地的表面密度(4.5 x 10（-7) / km(2)）比水星(9.9 x 10（-7) / km(2)）小两倍，这可能是它们的平均撞击速度（分别为19.4 km/s和42.5 km/s）差异很大以及峰环盆地开始直径差异的函数。对月球和类地行星上峰环盆地起始直径的新计算再次证实了先前的分析，即月球具有内太阳系中最大的峰环盆地起始直径。将峰环盆地形成模型的预测与月球新盆地目录的特征进行比较表明，内部熔体空洞的形成和改变以及撞击熔体体积随陨石坑直径的非线性缩放为峰环的发展提供了重要的控制因素。特别是，随着陨石坑直径的增加，内部熔化腔增长的幂律模型与月球和水星峰环盆地数据的幂律拟合是一致的。我们认为，熔融深度与瞬态空腔深度之间的关系对峰环盆地和多环盆地的直径及其后续发展提供了合理的控制，这与行星重力加速度和平均撞击速度在决定类地行星上盆地形态形成的重要作用是一致的。(C) 2011爱思唯尔公司版权所有。
Impact craters on planetary bodies transition with increasing size from simple, to complex, to peak-ring basins and finally to multi-ring basins. Important to understanding the relationship between complex craters with central peaks and multi-ring basins is the analysis of protobasins (exhibiting a rim crest and interior ring plus a central peak) and peak-ring basins (exhibiting a rim crest and an interior ring). New data have permitted improved portrayal and classification of these transitional features on the Moon. We used new 128 pixel/degree gridded topographic data from the Lunar Orbiter Laser Altimeter (LOLA) instrument onboard the Lunar Reconnaissance Orbiter, combined with image mosaics, to conduct a survey of craters >50 km in diameter on the Moon and to update the existing catalogs of lunar peak-ring basins and protobasins. Our updated catalog includes 17 peak-ring basins (rim-crest diameters range from 207 km to 582 km, geometric mean = 343 km) and 3 protobasins (137-170 km, geometric mean = 157 km). Several basins inferred to be multi-ring basins in prior studies (Apollo, Moscoviense, Grimaldi, Freundlich-Sharonov, Coulomb-Sarton, and Korolev) are now classified as peak-ring basins due to their similarities with lunar peak-ring basin morphologies and absence of definitive topographic ring structures greater than two in number. We also include in our catalog 23 craters exhibiting small ring-like clusters of peaks (50-205 km, geometric mean = 81 km); one (Humboldt) exhibits a rim-crest diameter and an interior morphology that may be uniquely transitional to the process of forming peak rings. A power-law fit to ring diameters (D-ring) and rim-crest diameters (D-r) of peak-ring basins on the Moon [D-ring = 0.14 +/- 0.10(D-r)(1.21 +/- 0.13)] reveals a trend that is very similar to a power-law fit to peak-ring basin diameters on Mercury [D-ring = 0.25 +/- 0.14(D-rim)(1.13 +/- 0.10)] [Baker, D.M.H. et al. [2011]. Planet. Space Sci., in press]. Plots of ring/rim-crest ratios versus rim-crest diameters for peak-ring basins and protobasins on the Moon also reveal a continuous, nonlinear trend that is similar to trends observed for Mercury and Venus and suggest that protobasins and peak-ring basins are parts of a continuum of basin morphologies. The surface density of peak-ring basins on the Moon (4.5 x 10(-7) per km(2)) is a factor of two less than Mercury (9.9 x 10(-7) per km(2)), which may be a function of their widely different mean impact velocities (19.4 km/s and 42.5 km/s, respectively) and differences in peak-ring basin onset diameters. New calculations of the onset diameter for peak-ring basins on the Moon and the terrestrial planets re-affirm previous analyses that the Moon has the largest onset diameter for peak-ring basins in the inner Solar System. Comparisons of the predictions of models for the formation of peak-ring basins with the characteristics of the new basin catalog for the Moon suggest that formation and modification of an interior melt cavity and nonlinear scaling of impact melt volume with crater diameter provide important controls on the development of peak rings. In particular, a power-law model of growth of an interior melt cavity with increasing crater diameter is consistent with power-law fits to the peak-ring basin data for the Moon and Mercury.We suggest that the relationship between the depth of melting and depth of the transient cavity offers a plausible control on the onet diameter and subsequent development of peak-ring basins and also multi-ring basins, which is consistent with both planetary gravitational acceleration and mean impact velocity being important in determining the onset of basin morphological forms on the terrestrial planets. (C) 2011 Elsevier Inc. All rights reserved.