Geochemistry of the Martian Meteorite GRV 99027

GRV 90027 is a Martian lherzolitic shergottites (L-S) containing poikilitic, non-poikilitic, and melted pocket components. GRV 99027 is mainly composed of olive (55 vol%) and pyroxene (37.5 vol%), with minor maskelynite (6 vol%) and chromite (1.5 vol%), and trace whitelockite and troilite, ect. In this paper, the mineralogy and petrology of GRV 99027 are reported; in addition, the geochemical characteristics of the REEs and H isotopes in the GRV 99027 are also further investigated. The ΣREE in GRV 99027 is relatively low; HREEs are enriched in olivine and pyroxene grains; LREEs are enriched in plagioclase with a high positive Eu anomaly. High ΣREE value is found in rare mineral whitlockite (less than 0.2 vol%), LREE≈HREE, and whitlockite has a negative Eu anomaly. The REE distribution patterns of the whole -rock of GRV 99027 is similar to but different from that of other L-S Martian meteorites, indicating that they came from different location of Mars. GRV 99027 has a high δD value. Different water-bearing minerals give different contribution for δD value. The δD of phosphates generally does not correlate with water content, and δD has a weak negative correlation with water content. GRV 99027 can be classified as an L-S Martian meteorite based on mineralogical assemblage patterns, REE distribution patterns, and hydrogen isotope. The isotope data of Sr, Nd, Pb, Os and REE from other L-S Martian meteorites were collected to discuss the formation history of the GRV 99027. Similar to other L-S Martian meteorites, GRV 99027 originated from part of Mar's mantle; during one strong impact event about 4M years ago, the meteorites were ejected from deep mantle into space, and traveled for a different duration in space (indicated by different cosmic exposure time), and captured by the Earth later in different time, ultimately falling on the Antarctica as L-S Martian meteorites.     

Meteorites from Grove Mountains, Antarctica:An overview

Thirty-two meteorites were collected in Grove Mountains area, Antarctica, by the 15th and 16th Chinese Antarctic Research Expeditions (CHINARE). Petrography and mineral chemistry of these meteorites are reviewed, among which there are one Martian lherzolite, one eucrite, one ungrouped iron meteorite, and six unequili-brated and twenty-three equilibrated ordinary chondrites. An equilibrated ordinary chondrite GRV 98004 ( H5 ) has an unusually low cosmic-ray exposure age. Meteorite concentrating processes in Grove Mountains area are discussed. In addition, future studies on Grove Mountains (GRV) meteorites are proposed.     

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基于深度置信网络的CRISM影像火星表面矿物识别方法

鉴于传统的光谱特征参数方法存在不能综合考虑光谱在整个波长范围内的谱形、对于单一吸收带相似的不同矿物难以区分等问题,研究采用深度置信网络方法对火星专用小型侦察影像频谱仪（CRISM）高光谱影像中的火星表面矿物进行自动识别,该算法具体包括:①预训练阶段。利用非监督算法逐层训练受限玻尔兹曼机,自动学习模型参数,提取光谱特征。②调优阶段。将自动学习的光谱特征输入分类器,采用反向传播算法对模型进行监督微调,识别矿物在CRISM影像中的分布。在算法的研究中,采用光谱比值方法降低火星表面灰尘等噪声对矿物光谱的影响,并探讨样本数量、隐含层节点数、网络深度等对算法识别精度的影响,试图构建适宜于CRISM影像火星表面矿物识别的深度置信网络模型。以火星表面镁铁蒙脱石和氯盐为例进行测试,实验结果表明:该方法能够对火星表面矿物进行自动识别,准确率达到85%以上,与光谱参数法的识别结果基本叠合,并能够探测光谱参数法未能识别的部分矿物分布。      

Subsurface target recognition in Utopia Planitia of Mars by Tianwen-1 FP-SPR simulation

As a cold and dry planet, Mars contains water resources in the form of water ice, so that the electromagnetic waves can be transmitted to the deep underground to get the information of the topography and subsurface geological structure. Subsurface penetrating radar(SPR) can be widely used in deep space exploration for a long time because of its non-destructive detection mode and its working characteristics not limited by visible light. It is an important type of equipment for detecting the subsurface structure of planets. Orbiter radar is mainly used in Mars exploration. However, because of its low resolution, it is difficult to describe the near surface structure, so there is a lack of radar data which can reflect the shallow information. In this paper, a three-dimensional near surface model of Utopia Planitia on Mars is established. In order to make the simulation results more reasonable, the key factors such as topographic relief, subsurface rocks and water ice, and the variation of dielectric constant in different layers are taken into account. Then the full polarization forward modeling is carried out by using the three-dimensional finite-difference time-domain method. The acquired full polarimetric subsurface penetrating radar(FP-SPR) data with noise is preprocessed and further processed by Pauli decomposition. The underground reflection can be picked up more clearly from the Pauli decomposition results. This work is helpful to identify more details of subsurface structures and provides a reference for the measured data in the future.     

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中国西部地壳垂直运动引起的重力场空间变化特征

结合中国西部区域的数字高程数据以及地壳垂直运动速率数据,计算中国西部地区地壳垂直运动引起的重力场变化的分布,并与卫星重力观测结果进行对比。研究表明：中国西部区域的重力场变化与地壳垂直运动速率场变化有很强的相关性,青藏高原以南的喜马拉雅山脉地壳上升运动速率最大,其引起的重力变化为正的最大值;准噶尔盆地地壳下沉运动速率最大,其引起的重力变化为负的最大值;塔里木盆地及柴达木盆地地壳下沉运动速率相对较小,相应地引起的重力变化值相对较小。