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The chemical compositions of silicate minerals, sulphide minerals and metal Fe-Ni in theQingzhen meteorite were measured by the microprobe analyses. Based upon these chemicalcompositions, the cosmochemical behaviour and characteristics of the existing forms of themajor elements in the Qinzhen meteorite have been discussed. These characteristics show thatunder the S-rich, O-poor, and strongly reducing conditions, the light metal elements, such asCa, Mg, K, Na may form sulphide, and metal Fe-Ni may contain Si and P. However, we con-sider that the light metal-sulphide can be stable in the lower mantle and there are some Siand P in the Fe-Ni core. Finally, an earth core-mantle model is established, where the Fe-Ni core contains some Si and P; the lower mantle is composed of Mg-rich silicate, SiO_2 andsulphide; the upper mantle, of silicate and oxide. 相似文献
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AQI指数(Air Quality Index)是传统的衡量空气质量状况好坏的标准之一.随着近年来管控治理污染物意识的提高,对AQI指数进行预测的讨论具有重要意义.长短期记忆神经网络(Long-Short Term Memory,LSTM)在时间序列预测上表现出优异的性能,在各类时间序列预测问题中被广泛使用.为此,以北... 相似文献
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黄土中微玻璃陨石和微玻璃球的发现与意义 总被引:6,自引:0,他引:6
首次在陆相沉积物-黄土中发现了16颗微玻璃陨石和3颗陨石消融型si-Mg微玻璃球。它们赋存于洛川黄土剖面中B/M界线之上,L8上部层位中,其沉降年龄为0.72—0.724Ma,与深海岩芯中澳-亚群微玻璃陨石的赋存层位一致,黄土中微玻璃陨石呈球状、椭球状、肾状、滴状及不规则状,颜色以微黄褐色,微黄绿色和浅黄棕色为主,少数为浅绿色、白色及无色透明球粒,粒径在65—220μm之间,多具溶蚀痕迹,但仍可见明显的气孔和凹坑,并发育有流动构造和熔渣构造。据其主量元素成分,黄土中微玻璃陨石可分为普通、瓶绿色和高铝微玻璃陨石三个化学群,其化学成分分别与深海岩芯中相同类型的微玻璃陨石相同。据其地理位置,赋存层位,沉降年龄及化学成分,这些黄土中微玻璃陨石属澳-亚散落群。微量元素研究表明,微玻璃陨石具有复杂的形成过程,其母源物质是多来源的。 相似文献
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可见光响应光催化剂K4Ce2Ta10O30、K4Ce2Nb10O30及其固溶体的电子结构 总被引:2,自引:0,他引:2
基于密度泛函理论(DFT), 采用平面波赝势(PWP)以及广义梯度近似(GGA)方法, 对可见光响应的光催化剂K4Ce2Ta10O30、K4Ce2Nb10O30及其固溶体进行电子结构的第一性原理计算. 结果表明, 光催化剂K4Ce2Ta10O30和K4Ce2Nb10O30的导带分别主要由Ta 5d和Nb 4d组成, 处于高能级的电子未占据态的Ce 4f与其有很明显的重迭, 但由于其高度局域特性,不能很好地参与光生电子在导带中的传导, 从而对光催化活性的贡献很小;而其价带则由O 2p与Ta 5d (Nb 4d)的杂化轨道组成, 同时电子占据态的Ce 4f对价带也有一定的贡献, 各个电子轨道对能带结构的贡献决定了该系列可见光响应光催化剂的物理化学和光催化特性. 固溶体系列中随着Nb含量的增加, 其吸收光谱依次红移, 带隙变窄, 导带底变低, 光生电子的还原能力降低. 在固溶体K4Ce2Ta10-xNbxO30(x=2, 5, 8)中, 由于Ce 4f轨道对价带顶的贡献相对较小, 固溶体的价带顶低于K4Ce2Ta10O30、K4Ce2Nb10O30的价带顶, 光生空穴的氧化能力相对较强. 该系列光催化剂的电子结构分析结果与光催化水分解的活性实验结果有很好的一致性. 相似文献
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月球微磁层的探测 总被引:1,自引:0,他引:1
近月空间环境中的等离子体特性是嫦娥一号及二号卫星的重要科学探测目标之一.基于嫦娥卫星上搭载的太阳风离子探测器(SWID)的测量结果,文章作者对月球表面磁异常结构(LMA)与太阳风相互作用这一空间科学中的热点问题进行了探索,并通过质子相空间分布的信息,初步确认了磁异常结构可以对入射原始太阳风起到屏蔽及加热的作用,形成所谓的"微磁层"结构.这是国际上为数不多的微磁层存在证据之一.文章作者期待这一研究(及后续工作)将不仅对月球表面空间风化效应的研究产生推动作用,同时也将有助于百公里尺度上(即质子回旋半径与宏观尺度相当条件下)的磁层物理学研究的发展. 相似文献
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Forty-four burk samples of the H chondrite Jilin have been analysed for their contents ofspallogenic, trapped and radiogenic noble gases, and thirty-five samples have been determinedfor their radiocosmogenic nuclides. The Jilin meteorite has an extreme complicated history ofcosmic-ray irradiation. In the 1st-stage, the Jilin meteorite might be located between 0.2--2mbelow the surface of the parent body travelling about 8 m. y. in space and under a geometryof 2π subjected to the radiation of cosmic-ray. According to the data of ~(60)Co dating the burialdepth of all samples in the 2nd-stage can be determined and the preatmospheric form andsize of the parent body can be restored (under a geometry of 4π). The result of this recon-struction is that, the 2nd-stage has a nearly spheric form, with a radius of 85±5 cm, weighing9.7±1.7 Ts. The position of the center of the preatmospheric body is: X=55, Y=55 andZ=39. Jilin meteorite No.1 is located at the center of the parent body and is surroundedwith the fragments. The ablation rate is estimated at about 30%. We have proposed a new modelof the two-stage irradiation, and based on the contents of ~(21)Ne-~(60)Co in the samples, a classificationscheme can be worked out for the restoration of relative position of the samples within theparent body. 相似文献
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The comparison of Raman spectra of the chondrites (C, H, L, LL) has confirmed thatthere exist two types of meteorite carbon: one is the primary carbon present in carbonaceouschondrites (c) and the other is the secondary carbon contained in ordinary chondrites (H, L,LL). The parameter of order (I_G/I_D intensity ratio, similarly hereinafter) of primary car-bon tends to decrease with increasing petrologic type and it can reflect the temperature ofdust carrier at the time plasma gases in the early nebula were condensed to form primarycarbonaceous material and the hydrogen content in primary carbonaceous material. This kindof primary carbonaceous material maybe has not experienced late stage thermometamorphismwithin the parent body of chondrites, indicating that the carbonaceous chondrites wereformed and retained in the low temperature region of the solar system. The parameter oforder of the secondary carbon tends to increase with increasing petrologic type and it can re-flect the degree of graphitization o 相似文献
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