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华北克拉通破坏存在空间上的差异性,至今其内在的动力学机制仍存在较大的争议,这种差异性在岩石圈热结构上必然有所表现.广义上岩石圈热结构包括热流结构、温度场结构和热岩石圈厚度,是揭示岩石圈演化及其内在动力学过程的重要基础.基于二维地震剖面和大地热流数据,建立二维稳态热传导有限元模型,对华北克拉通东部岩石圈热结构进行模拟计算并与西部进行对比分析,在此基础上对比热岩石圈与地震岩石圈厚度差异的变化.结果显示,华北克拉通东、西部岩石圈热结构有着较为明显的差异,地幔热流值波动范围分别在24~44/20.5~24.5mW·m~(-2),壳幔比1.61~0.70/1.84~1.51,以1300℃等温线计算得到的热岩石圈厚度变化范围在75~139km/128~162km.华北克拉通东部相对西部有着较高的深部地幔热流值和较小的地震/热岩石圈厚度差异,这可能意味着东部软流圈地幔有效黏度相比西部低,估算差异可达2~3个数量级. 相似文献
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本文利用瑞利波群速度频散资料和层析成像方法,研究了中国西部及邻近区域(20°N—55°N,65°E—110°E)的岩石圈S波速度结构.结果表明这一地区存在三个以低速地壳/上地幔为特征的构造活动区域:西蒙古高原—贝加尔地区,青藏高原,印支地区.西蒙古高原岩石圈厚度约为80 km,上地幔低速层向下延伸至300 km深度,说明存在源自地幔深部的热流活动.缅甸弧后的上地幔低速层下至200 km深度,显然与印度板块向东俯冲引起俯冲板片上方的热/化学活动有关.青藏高原地壳厚达70 km,边缘地区厚度也在50 km以上并且具有很大的水平变化梯度,与高原平顶陡边的地形特征一致.中下地壳的平均S波速度明显低于正常大陆地壳,在中地壳20~40 km深度范围广泛存在速度逆转的低速层,这一低速层的展布范围与高原的范围相符.这些特征说明青藏高原中下地壳的变形是在印度板块的北向挤压下发生塑性增厚和侧向流动.地幔的速度结构呈现与地壳显著不同的特点.在高原主体和川滇西部地区上地幔顶部存在较大范围的低速,低速区范围随深度迅速减小;100 km以下滇西低速消失,150 km以下基本完全消失.青藏高原上地幔速度结构沿东西方向表现出显著的分段变化.在大约84°E以西的喀喇昆仑—帕米尔—兴都库什地区,印度板块的北向和亚洲板块的南向俯冲造成上地幔显著高速;84°E—94°E之间上地幔顶部速度较低,在大约150~220 km深度范围存在高速板片,有可能是俯冲的印度岩石圈,其前缘到达昆仑—巴颜喀拉之下;在喜马拉雅东构造结以北区域,存在显著的上地幔高速区,可能阻碍上地幔物质的东向运动.川滇西部岩石圈底界深度与扬子克拉通相似,约为180 km,但上地幔顶部速度较低.这些现象表明青藏高原岩石圈地幔的变形/运动方式可能与地壳有本质的区别. 相似文献
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莫霍面是地壳和上地幔的边界,但莫霍面并不是一个简单的"面",而是一个反映地壳和地幔物质交换、相互作用等动力学意义的"过渡带".本文综合深地震反射、宽角地震折射和高温高压岩石物理实验结果,确定壳-幔过渡带的地震P波速度变化范围为6.8~7.5 km·s-1.在克拉通等构造活动稳定地区壳-幔过渡带内的速度梯度强且壳-幔过渡带厚度薄,而在造山带等构造活动区域壳-幔过渡带内的速度梯度弱且壳-幔过渡带厚.中国东部地区的壳-幔过渡带的平均厚度约为5~10 km,在四川盆地下方最薄（<5 km）,而在华北克拉通中部造山带下方的壳-幔过渡带最厚（~30 km）.综合地球化学结果,华北中部巨厚壳-幔过渡带主要是幔源岩浆的底侵作用和堆晶作用而形成. 相似文献
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本文利用宽频流动台阵记录的远震波形资料和接收函数波动方程叠后偏移方法,获得了华北克拉通东北部边界及其邻近地区的地壳和地幔转换带的间断面结构图像.结果显示研究区域的地壳厚度存在显著的横向变化:以南北重力梯度带为界,西北部的兴蒙造山带地壳较厚(~40 km),东南部的燕山带、松辽盆地和辽东台隆地壳明显较薄(30~35 km).这有可能反映,研究区南北重力梯度带两侧地壳在中-新生代区域构造伸展过程中经历了不同程度的改造和减薄.地幔转换带成像结果显示,研究区410 km和660 km间断面结构存在横向差异.经度121°E-122°E之间,上地幔底部出现双重间断面,深度分别为660 km和690 km.经度122.5°E以东(北黄海地区),410 km间断面有5~20 km幅度的下沉,660 km间断面有5~15 km幅度的抬升;该地区地幔转换带厚度相对全球平均偏薄10~20 km,指示着该地区较热的上地幔底部温度环境.我们认为太平洋俯冲板块可能停滞在研究区119°E-122°E经度范围的地幔转换带中,但未延伸至118°E以西;而俯冲板块在124°E以东可能局部穿透了上地幔底部而进入下地幔,同时引起小尺度的地幔对流,导致北黄海地区下地幔物质的上涌. 相似文献
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月球表层与月壳岩石密度的横向与径向的变化,反映了月表及内部成分以及月球演化等特征.本文利用月球勘探者号伽马射线谱仪探测的月表Fe, Th与Mg元素分布数据,依据前人给出的元素含量与岩石类型的关系,对月球表层进行了岩性填图,并结合岩石样品与陨石的密度测试数据建立初始密度模型,采用铁元素与岩石密度的关系对其进行修正,从而建立了月表物质密度分布模型.基于嫦娥一号激光测高数据和日本SELENE计划发布的月球重力模型,计算出月球布格重力异常,进而反演得到月壳0~40 km深度范围内岩石平均密度分布模型.分析表明,大部分区域上,月壳至少月壳上部岩石成分主要以轻质的富含铝、钙、镁质的硅酸盐类岩石为主.由此推测,原始月壳极有可能是由轻质的、富含钙、镁质硅酸盐类岩石构成的全球性月壳.现今的玄武岩与克里普岩只是覆盖于原始的月壳之上的岩层,且厚度不大. 相似文献
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莫霍面是地壳和上地幔的分界面，是个重要的密度界面，东海莫霍面的展布特征，对于研究东海深部构造具有重要意义.利用最新重力异常数据反演莫霍面深度，结合前人的莫霍面深度结果，分析东海及其邻域的壳－幔结构与展布特征.从莫霍面深度图可见东海及其邻域莫霍面起伏变化很大，深度在12～34 km之间变化，东海及其邻域地壳厚度为6～34km，东海陆架地区地壳厚度变化与大陆地区相比并不明显，显著减薄开始于冲绳海槽地区，琉球岛弧处地壳厚度明显再度增加，莫霍面呈现两凹两凸形态，认为东海及其邻域地壳自西而东从陆壳－过渡壳－洋壳逐渐过渡的. 相似文献
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上地幔温度是控制地幔流变性和动力学过程的关键参数之一.本文利用高分辨率S波地震层析成像速度结果,基于岩石温度与地震波速度的关系,研究了华北地区上地幔50~300 km深度范围内的温度分布和"热"岩石圈厚度.为了验证结果的可靠性,本文用计算的上地幔60 km深度处的温度作为底面约束,得到了相应的地表热流.计算地表热流与观测地表热流之间符合程度较好,相对误差大部分都在地表热流观测误差范围之内.通过对上地幔的温度分布进行分析,我们研究发现:(1)在上地幔浅部,温度与地表构造之间有很好的对应关系.在小于170 km的深度上,温度呈现东高西低的分布态势.温度较高的区域集中在东部的河淮盆地、渤海湾盆地、华北平原和中部陆块的交界处、西部鄂尔多斯高原北缘的银川―河套地堑以及阴山地区,同时,这些地区的岩石圈厚度也相应较薄,大约为80~100 km;(2)西部的鄂尔多斯高原是整个华北地区岩石圈地幔温度最低的地区,比东部地区低200~400 ℃,岩石圈厚度相应最厚,平均岩石圈厚度达到140~150 km,最厚处超过160 km.(3)在170 km以下的软流圈地幔部分,温度分布发生反转,西部温度高于东部,表明东、西部陆块在地质历史时期经历了不同的深部地幔动力学过程. 相似文献
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《地球物理学进展》2015,(3)
OBS2013测线沿NNW-SSE方向跨越渤中坳陷和胶东隆起次级构造以及张家口-蓬莱和郯庐两条深大断裂带.对测线上13个站位折合剖面进行震相分析,识别出丰富的Ps、Pg、PcP、Pn和PmP震相.通过射线追踪和走时拟合,建立了二维P波速度结构模型.模型将渤海深部速度结构分为6层,最上部两层为新生界,速度由1.8~2.0km/s变化为4.4~4.7km/s,埋深为0.5~7.2km,并向胶东隆起方向逐渐尖灭.向下依次分为上地壳下部、中地壳和下部地壳,地壳速度由5.6~5.9km/s变化为7.0km/s,其中上地壳底界面埋深11.1~12.9km,中地壳底界面埋深18.0~18.9km,莫霍面在渤中凹陷处埋深最浅为25.5km,向胶东隆起方向逐渐增大到30km.莫霍面之下上地幔顶部速度为8.0~8.1km/s.渤海下部地壳厚度变化接近5km,从下地壳到上地幔顶部均无明显的大尺度横向速度变化,岩浆底侵不发育.结合已有研究成果,推测渤海东南部与华北克拉通中部相比,下地壳厚度减薄9~13.4km,地壳减薄非常有限,具有典型陆壳特征. 相似文献
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在频域使用多窗口(Multitaper)方法来计算月球正面四个形成于不同历史时期月海区(Smythii, Crisium, Imbrium, Orientale)的重力地形导纳,然后将其与月球弹性岩石圈的理论导纳模型相比较,由最小二乘法得出四个月海区的月球岩石圈的平均弹性厚度约为8 km,月壳的厚度分别为：Smythii 盆地,72 km; Crisium 盆地 70 km;Orientale 盆地 60 km;Imbrium 盆地57 km.随着月球的演化,月壳厚度呈现变厚的趋势. 相似文献
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The composition, structure and evolution of the moon's interior are narrowly constrained by a large assortment of physical and chemical data. Models of the thermal evolution of the moon that fit the chronology of igneous activity on the lunar surface, the stress history of the lunar lithosphere implied by the presence of mascons, and the surface concentrations of radioactive elements, involve extensive differentiation early in lunar history. This differentiation may be the result of rapid accretion and large-scale melting or of primary chemical layering during accretion; differences in present-day temperatures for these two possibilities are significant only in the inner 1000 km of the moon and may not be resolvable. If the Apollo 15 heat-flow result is representative of the moon, the average uranium concentration in the moon is 0.05–0.08 p.p.m.Density models for the moon, including the effects of temperature and pressure, can be made to satisfy the mass and moment of inertia of the moon and the presence of a low-density crust inferred from seismic refraction studies only if the lunar mantle is chemically or mineralogically inhomogeneous. The upper mantle must exceed the density of the lower mantle at similar conditions by at least 5%. The average mantle density is that of a pyroxenite or olivine pyroxenite, though the density of the upper mantle may exceed 3.5 g/cm3. The density of the lower mantle is less than that of the combined crust and upper mantle at similar temperature and pressure, thus reinforcing arguments for early moon-wide differentiation of both major and minor elements. The suggested density inversion is gravitationally unstable and implies stresses in the mantle 2–5 times those associated with the lunar gravitational field, a difficulty that can be explained or avoided by: (1) adopting lower values for the moment of inertia and/or crustal thickness, or (2) postulating that the strength of the lower mantle increases with depth or with time, either of which is possible for certain combinations of composition and thermal evolution.A small iron-rich core in the moon cannot be excluded by the moon's mass and moment of inertia. If such a core were molten at the time lunar surface rocks acquired remanent magnetization, then thermal-history models with initially cold interiors strongly depleted in radioactive heat sources as a primary accretional feature must be excluded. Further, the presence of ～||pre|40 K in a FeFeS core could significantly alter the thermal evolution and estimated present-day temperatures of the deep lunar interior. 相似文献
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月表太阳辐射是深入研究月表温度分布的关键问题之一. 本文根据月表有效太阳辐照度与太阳常数、太阳辐射入射角以及日月距离之间的关系,建立月表有效太阳辐照度的实时模型. 该模型在1950～2050年的100年内的理论误差百分比小于0.28％, 相对前人提出的模型在精度上有了很大程度的提高,能较为真实地反映月表有效太阳辐照度随时间的变化规律. 计算结果表明2007年月表太阳辐照度的年变化范围在1321.5～1416.6 W·m-2之间,平均为1368.0 W·m-2. 通过对月表太阳辐射入射角计算结果的分析,证实了月球的两极可能存在极昼极夜. 相似文献
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We model the internal structure of the Moon, initially homogeneous and later differentiated due to partial melting. The chemical
composition and the internal structure of the Moon are retrieved by the Monte-Carlo inversion of the gravity (the mass and
the moment of inertia), seismic (compressional and shear velocities), and petrological (balance equations) data. For the computation
of phase equilibrium relations and physical properties, we have used a method of minimization of the Gibbs free energy combined
with a Mie-Gr@uneisen equation of state within the CaO-FeO-MgO-Al2O3-SiO2 system. The lunar models with a different degree of constraints on the solution are considered. For all models, the geophysically
and geochemically permissible ranges of seismic velocities and concentrations in three mantle zones and the sizes of Fe-10%S
core are estimated. The lunar mantle is chemically stratified; different mantle zones, where orthopyroxene is the dominant
phase, have different concentrations of FeO, Al2O3, and CaO. The silicate portion of the Moon (crust + mantle) may contain 3.5–5.5% Al2O3 and 10.5–12.5% FeO. The chemical boundary between the middle and the lower mantle lies at a depth of 620–750 km. The lunar
models with and without a chemical boundary at a depth of 250–300 km are both possible. The main parameters of the crust,
the mantle, and the core of the Moon are estimated. At the depths of the lower mantle, the P and S velocities range from 7.88 to 8.10 km/s and from 4.40 to 4.55 km/s, respectively. The radius of a Fe-10%S core is 340 ± 30
km. 相似文献
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Inferences on the lunar temperature regime are made from the inversion of gravity for density anomalies and the stress-state of the Moon's interior, and by comparing these results with flow laws and estimates of likely strain-rates.The nature of the spectrum of the lunar gravitational potential indicates that the density anomalies giving rise to the potential are mainly of near-surface origon. The average stress-differences in the lunar mantle required to support these density anomalies are of the order of a few tens of bars and have persisted for more than 3 · 109 years. If current flow laws for dry olivine can be extrapolated to the conditions of the lunar mantle, and the selenotherms based on electrical conductivity models are valid, the strain rates are too high to explain the preservation of the lateral near-surface density anomalies. We suggest that the present temperatures in the Moon are relatively low, of the order of 800°C or less, at a depth of about 300 km. This compares with 1100°C based on electrical conductivity models and is near the lower limit predicted by Keihm and Langseth (1977) from lunar heat-flow observations. 相似文献
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Variation of crustal thickness in the Philippine Sea deduced from three-dimensional gravity modeling
Abstract Crustal thickness of the northern to central Philippine Sea was gravimetrically determined on the simple assumption of four layers: seawater, sediments, crust and lithospheric mantle, with densities of 1030, 2300, 2800 and 3300 kg/m3 , respectively. As for the correction of the regional gravity variation, a 15 km difference of the lithospheric thickness with a density difference of 50 kg/m3 against the asthenosphere below between both sides of the Kyushu-Palau Ridge was taken into consideration. Mantle Bouguer anomalies were calculated on the assumption of constant crustal thickness of 6 km, and then the crustal thickness was obtained by three-dimensional gravity inversion method. The results show occurrence of thin crust areas with a thickness of approximately 5 km in the southern part and at the western margin of the Shikoku Basin and also of thick crust areas in the northwestern and northeastern parts of the Parece Vela Basin. We suggest that these are because of the variation of magma supply at the time of sea floor spreading in the Shikoku and Parece Vela Basins, which is possibly related to the variation of spreading rate and enhanced magmatism near the past arc volcanic fronts. The results further show the occurrence of crust thinner than 5 km in the northeastern part of the West Philippine Basin, of crust thicker than 15 km in the Amami Plateau, the Daito and Oki-Daito Ridges, and also in the northern part of Kyushu-Palau Ridge, whereas the southern part of the Kyushu-Palau Ridge the crust is thicker than 10 km. It was also inferred that small basins in the Daito Ridge province have the thinnest oceanic crust of less than 5 km in the Kita-Daito Basin. 相似文献
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西沙地块作为在南海形成演化过程中形成的微陆块,记录了南海演化历史的重要信息,其地壳结构、物质组成及构造属性是探讨南海形成演化的关键.基于采集到的OBS2013-3测线海底地震仪数据,用射线追踪和正演走时拟合方法,获得了西沙地块的二维纵波速度模型.模型显示沉积层速度为2.2~3.2km·s-1,厚度为0.8~3.0km,局部基底面起伏较大,上地壳顶部速度为5.0~5.5km·s-1,下地壳底部速度为6.9km·s-1,上地幔顶部速度为8.0km·s-1.西沙地块的地壳厚度平均为23km,上地壳厚度约为9km,下地壳厚度约为14km,莫霍面埋深为23~27km.从穿过西沙地块的纵、横两条大剖面推算,块体大小约为9.2×105 km3,与华南陆缘相比,表现为整体减薄的陆壳特征.西沙地块与南沙地块垂直于西南次海盆扩张脊分布,根据二者地壳结构的特征对比,二者互为共轭关系. 相似文献
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俯冲板块的深部脱水使得上覆地幔含水, 从而降低含水地幔的熔点, 导致上覆地幔部分熔融。 部分熔融的地幔柱一旦喷发到地表就是俯冲带火山, 也形成新的地壳。 相对于周围的地幔来讲, 具有较小密度和黏度的部分熔融地幔的时空活动性就控制着俯冲带火山的时空分布特征。 本文主要回顾近年来运用三维热力学岩石力学模型数值模拟研究与板片脱水相关的俯冲带火山活动的时空分布特性。 结果表明, 部分熔融地幔的有效黏度和密度是影响俯冲板片之上的三维地幔柱横向分布特征的主要因素。 高黏度的部分熔融地幔(1020~1021 Pa·s )易于形成近平行于海沟的、 长波长(70~100 km)的、 薄的波状地幔柱; 低黏度(1018~1019 Pa·s )的熔融地幔易于形成平行于海沟的, 短波长(30~50 km)的蘑菇状地幔柱和垂直于海沟的山脊状地幔柱。 当部分熔融地幔和周围地幔的密度相差小于50 kg/m3时, 在俯冲板片之上只能形成长波长低幅度(宽50~100 km, 高10~15 km)的地幔山丘。 岩浆产率随着时间的变化反映了火山活动的生命周期性。 板块俯冲速度会影响地幔柱形成的深度和范围大小。 高效率熔融提取会增加新地壳增长总量。 低的板块俯冲速度和低的熔融提取效率会增加上地壳(花岗岩质)和中地壳(英安岩质)化学成分的比例。 数值模拟结果可以很好地解释如日本东北、 新西兰、 南阿拉斯加俯冲区火山的横向分布特征。 相似文献
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J.Peter Watt 《Physics of the Earth and Planetary Interiors》1981,25(1):57-63
Mean atomic weight profiles for the lunar mantle have been calculated from velocity-density systematic relations using lunar density and seismic velocity models. Despite large variability among the models, the calculation including Poisson's ratio yields a range of mean atomic weight values between 22 and 23 g mol?1 below 150 km. A similar calculation for the Earth's mantle produces a mean atomic weight of 21.1 ±0.4 g mol?1. This suggests that the Moon cannot be derived directly from the Earth's mantle, or that it has had a differentiation history different from the Earth's. The lunar require an Fe mole fraction between 0.25 and 0.33 for a pure olivine mantle, or between 0.33 and 0.45 for pure pyroxene.The present profiles are 0.5–3.0 g mol?1 higher than those calculated from lunar compositional models based on lunar rock compositions and petrology and assumed lunar histories, indicating inadequacies in either the seismic or compositional models, or in both. The mean atomic weight approach provides a method of comparing the consistency of seismic and compositional models of planetary interiors. 相似文献