Small-scale lunar farside volcanism
Small-scale lunar farside volcanism
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DOI：
10.1016/j.icarus.2015.04.040
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发表时间：
2015-09
期刊：
影响因子：
3.2
通讯作者：
J. Pasckert;H. Hiesinger;C. H. Bogert
中科院分区：
文献类型：
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作者：
J. Pasckert;H. Hiesinger;C. H. Bogert
我们确定并绘制了28月海玄武岩的出现，南方和南极艾特肯盆地之间的月球背面，并确定其绝对模型年龄（AMAs）进行陨石坑的大小频率分布（CSFD）的测量。我们的研究区域可以细分为七个主要的月海玄武岩发生在Bolyai，Roche V，Rosseland，Pauli和Roche陨石坑及其周围，Rosseland和Coblentz陨石坑以南，以及Eötvös和Roche陨石坑之间的月海斑块。Bolyai陨石坑内和周围的月海玄武岩的AMA范围从2.1 Ga到3.5 Ga（两个单位），在短距离内变化很大。科布伦茨陨石坑南部的月海斑块包含9个单元，其AMA范围从2.1 Ga到3.8 Ga。Roche V陨石坑的月海玄武岩的AMA值为2.2Ga。我们绘制了七个火山单位在Rosseland陨石坑和派生AMA为这些单位中的五个。罗斯兰陨石坑中的月海玄武岩显示了我们研究区域发现的最年轻的AMA，范围从1.5 Ga到2.9 Ga。Rosseland火山口南部的月海玄武岩显示出明显的年龄，AMA为3.3 Ga。Pauli和Roche陨石坑中的月海玄武岩显示出1.7 Ga至3.1 Ga的AMA。Eötvös和Roche陨石坑之间的月海斑块显示出类似的AMA范围，从1.9 Ga到3.1 Ga。在我们的研究中，月海玄武岩的AMA表明，月球背面的火山活动几乎与月球近面一样长（1.2 Ga前），或者至少比以前认为的（2.5 Ga前）更长，并通过月球玄武岩的上升和喷发模型预测。此外，我们还计算了所调查的月海玄武岩的厚度和体积。月海玄武岩的厚度在21 ~ 172 m之间，体积在0.1 ~ 379 km 3之间，与月球近、远面的月海玄武岩相似，具有很大的尺度范围。
We identified and mapped 28 mare basalt occurrences, between the Australe and South Pole-Aitken basins on the southern lunar farside, and determined their absolute model ages (AMAs) by performing crater size–frequency distribution (CSFD) measurements. Our study area can be subdivided into seven major mare basalt occurrences in and around Bolyai, Roche V, Rosseland, Pauli, and Roche craters, south of both Rosseland and Coblentz craters, as well as mare patches between Eötvös and Roche craters. The AMAs of the mare basalts in and around Bolyai crater range from 2.1 Ga to 3.5 Ga (two units), varying drastically within short distances. The mare patches south of Coblentz crater contain nine units that have AMAs ranging from 2.1 Ga to 3.8 Ga. The mare basalts in Roche V crater show an AMA of 2.2 Ga. We mapped seven volcanic units in Rosseland crater and derived AMAs for five of these units. The mare basalts in Rosseland crater show the youngest AMAs found in our study area, ranging from 1.5 Ga to 2.9 Ga. The mare basalt occurrence south of Rosseland crater shows significantly older ages with an AMA of 3.3 Ga. The mare basalts in Pauli and Roche craters show AMAs from 1.7 Ga to 3.1 Ga. The mare patches between Eötvös and Roche craters show a similar range of AMAs from 1.9 Ga to 3.1 Ga. The AMAs of the mare basalts in our study show that the lunar farside was volcanically active for nearly as long as the lunar nearside (1.2 Ga ago), or at least longer than previously thought (2.5 Ga ago) and predicted by models of the ascent and eruption of lunar basalts. In addition, we calculated thicknesses and volumes of the investigated mare basalts. With thicknesses between ∼21 m and ∼172 m and volumes from ∼0.1 km3to ∼379 km3, the mare basalts in our study area show a wide range of dimensions, similar to other mare basalts of the lunar near- and farsides.