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1.
Vladimir A.SANKOV Anna V.PARFEEVETS Andrey I.MIROSHNITCHENKO Aleksey V.SANKOV Amgalan BAYASGALAN Sodnomsambuu DEMBEREL 《地学前缘》2022,29(1):245-265
阿穆尔板块西部边界在蒙古境内的空间位置尚不清楚,并且活动断层构造及其沿线地壳的应力状态研究较少。本文在沿此边界的三个区域——杭爱—肯特构造鞍部、布尔古特地块(鄂尔浑—土拉交汇处)和色楞格地块(包括色楞格凹陷和布伦—努鲁隆起),利用空间图像解译、地形起伏度分析、地质构造资料以及构造压裂和沿裂缝位移资料重建构造古应力,对活动断层进行研究。研究表明,活动断裂继承了古生代和中生代古构造的非均质性。这些断层沿着板块边界并不是单一的带,而是成簇的。它们的运动取决于走向:亚纬向断层是具有一定逆分量的左旋走滑断层,北西向断层是逆断层或逆冲断层,通常具有右旋走滑分量,海底断层是右旋走滑断层,北东向断层是正断层。位于色楞格凹陷和杭爱东部的断裂构造的活动始于上新世。逆断层和走滑断层与上新世情况不符,但多与更新世地貌相符,表明其活动年代较晚,为更新世时期。利用构造断裂和沿断裂的位移,重建活动断裂带变形末阶段的应力应变状态,结果表明断裂在最大挤压轴的北北东和北东方向上以压缩和走滑为主。只有在色楞格凹陷内,以扩张和走滑类型的应力张量为主,且在最小挤压轴的北西走向尤为显著。在南部,杭爱东部(鄂尔浑地堑)内有1个以扩张机制为主的局部区域,说明蒙古中部断裂在更新世—全新世阶段的活动以及现代地震活动主要受与印度斯坦和欧亚大陆汇聚过程相关的东北方向的附加水平挤压的控制。使研究区地壳产生走滑变形、贝加尔湖裂谷发散活动以及阿穆尔板块东南运动的另一个因素是东南方向软流圈流动对岩石圈底部的影响。阿穆尔板块和蒙古地块之间的边界在构造结构上是零碎的,代表了覆盖整个蒙古西部变形带的边缘部分。 相似文献
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Fluid flow in many hydrocarbon reservoirs is controlled by aligned fractures which make the medium anisotropic on the scale of seismic wavelength. Applying the linear‐slip theory, we investigate seismic signatures of the effective medium produced by a single set of ‘general’ vertical fractures embedded in a purely isotropic host rock. The generality of our fracture model means the allowance for coupling between the normal (to the fracture plane) stress and the tangential jump in displacement (and vice versa). Despite its low (triclinic) symmetry, the medium is described by just nine independent effective parameters and possesses several distinct features which help to identify the physical model and estimate the fracture compliances and background velocities. For example, the polarization vector of the vertically propagating fast shear wave S1 and the semi‐major axis of the S1‐wave normal‐moveout (NMO) ellipse from a horizontal reflector always point in the direction of the fracture strike. Moreover, for the S1‐wave both the vertical velocity and the NMO velocity along the fractures are equal to the shear‐wave velocity in the host rock. Analysis of seismic signatures in the limit of small fracture weaknesses allows us to select the input data needed for unambiguous fracture characterization. The fracture and background parameters can be estimated using the NMO ellipses from horizontal reflectors and vertical velocities of P‐waves and two split S‐waves, combined with a portion of the P‐wave slowness surface reconstructed from multi‐azimuth walkaway vertical seismic profiling (VSP) data. The stability of the parameter‐estimation procedure is verified by performing non‐linear inversion based on the exact equations. 相似文献
4.
Fundamental differences between SPH and grid methods 总被引：1，自引：0，他引：1
Oscar Agertz Ben Moore Joachim Stadel Doug Potter Francesco Miniati Justin Read Lucio Mayer Artur Gawryszczak rey Kravtsov Åke Nordlund Frazer Pearce Vicent Quilis Douglas Rudd Volker Springel James Stone Elizabeth Tasker Romain Teyssier James Wadsley Rolf Walder 《Monthly notices of the Royal Astronomical Society》2007,380(3):963-978
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Paul A. Boley rey M. Sobolev Vadim V. Krushinsky Roy van Boekel Thomas Henning Aleksei V. Moiseev Maksim V. Yushkin 《Monthly notices of the Royal Astronomical Society》2009,399(2):778-782
The intent of this study is to determine the nature of the star and associated nebulosity S 235 B, which are located in a region of active star formation still heavily obscured by the parent molecular cloud. Low-resolution ( R = 400) long-slit spectra of the star and nebulosity, and medium- ( R = 1800) and high-resolution ( R = 60 000) spectra of the central star are presented along with the results of Fabry–Perot interferometric imaging of the entire region. Based on the long-slit and Fabry–Perot observations, the nebulosity appears to be entirely reflective in nature, with the stellar component S 235 B★ providing most of the illuminating flux. The stellar source itself is classified here as a B1V star, with emission-line profiles indicative of an accretion disc. S 235 B★ thus belongs to the relatively rare class of early-type Hebrig Be stars. Based on the intensity of the reflected component, it is concluded that the accretion disc must be viewed nearly edge-on. Estimates of the accretion rate of S 235 B★ from the width of the Hα profile at 10 per cent of maximum intensity, a method which has been used lately for T Tauri stars and Brown Dwarfs, appear to be inconsistent with the mass outflow rate and accretion rate implied from previous infrared observations by Felli et al., suggesting this empirical law does not extend to higher masses. 相似文献
6.
Geodetic observations of ice flow velocities over the southern part of subglacial Lake Vostok, Antarctica, and their glaciological implications 总被引：1，自引：0，他引：1
Jens Wendt Reinhard Dietrich Mathias Fritsche Anja Wendt Alexander Yuskevich rey Kokhanov Anton Senatorov Valery Lukin Kazuo Shibuya Koichiro Doi 《Geophysical Journal International》2006,166(3):991-998
In the austral summer seasons 2001/02 and 2002/03, Global Positioning System (GPS) data were collected in the vicinity of Vostok Station to determine ice flow velocities over Lake Vostok. Ten GPS sites are located within a radius of 30 km around Vostok Station on floating ice as well as on grounded ice to the east and to the west of the lake. Additionally, a local deformation network around the ice core drilling site 5G-1 was installed.
The derived ice flow velocity for Vostok Station is 2.00 m a−1 ± 0.01 m a−1 . Along the flowline of Vostok Station an extension rate of about 10−5 a−1 (equivalent to 1 cm km−1 a−1 ) was determined. This significant velocity gradient results in a new estimate of 28 700 years for the transit time of an ice particle along the Vostok flowline from the bedrock ridge in the southwest of the lake to the eastern shoreline. With these lower velocities compared to earlier studies and, hence, larger transit times the basal accretion rate is estimated to be 4 mm a−1 along a portion of the Vostok flowline. An assessment of the local accretion rate at Vostok Station using the observed geodetic quantities yields an accretion rate in the same order of magnitude. Furthermore, the comparison of our geodetic observations with results inferred from ice-penetrating radar data indicates that the ice flow may not have changed significantly for several thousand years. 相似文献
The derived ice flow velocity for Vostok Station is 2.00 m a
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冻融循环是影响寒区工程和环境变化的重要因素之一,而年冻融频次(冻融循环的年累计量)是可以直接标定冻融循环对寒区工程和环境造成影响大小的物理量,对寒区环境下年冻融频次的调查有重要意义。以中国东北兴安岭地区为研究对象,选取兴安岭地区18个气象站点1990—2017年地表温度数据进行整理,得出兴安岭地区各个站点的年冻融频次,并在空间分布和时间序列上分析了年冻融频次的变化情况。结果表明:年冻融频次在中国东北兴安岭地区随着纬度增加逐渐增多,随着经度的增加逐渐减少,随着海拔升高而逐渐增多,且均具有良好的线性趋势;年冻融频次在1990—2017年呈明显的减少趋势,在2004年前后发生突变。进一步分析发现,在影响年冻融频次空间分布的3个因素中,经纬度影响较大,海拔影响相对较小;在时间上年冻融频次变化与东北地区NDVI变化情况呈现良好的负相关性,表明年冻融频次在一定程度上与当地植被覆盖度有关,且随植被覆盖度的增加而减少。 相似文献
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球模仪测试冻土松弛模量的非线性Kelvin解答及其试验研究 总被引：1，自引：1，他引：0
冻土的松弛模量是进行蠕变力学分析的关键参数。但在理论方面, 尚未基于球模仪试验建立较完善的松弛模量表征公式。基于半空间黏弹性理论和分数阶微积分理论, 获得了松弛模量公式的非线性Kelvin模型解答并进行了材料参数影响分析。在给出恒载条件下, 可以用单轴蠕变试验的分析结果评估基于球形压痕试验的冻土松弛模量来预测准确性。随后分别以冻结细砂的球模仪试验曲线、 冻结砂和冻结砂质黏土的单轴蠕变曲线为例, 预测了各条试验曲线和冻土的松弛模量, 并通过其他试验实测数据进行了检验。结果表明： 该松弛模量表征公式的材料参数最少, 随各材料参数变化具有较佳单调性; 基于球形模板试验, 非线性Kelvin解答能对冻结细砂的松弛模量和位移曲线做出合理可靠的预测。非线性Kelvin模型能很好地吻合单轴蠕变试验曲线, 基于单轴蠕变试验的冻结砂松弛模量随时间变化规律和数值范围与球模仪试验分析结果较一致, 冻结砂质黏土的松弛模量随应力和温度的变化规律再现了已有研究结论。 相似文献
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Alexander Knebe rey V. Kravtsov † Stefan Gottlöber Anatoly A. Klypin 《Monthly notices of the Royal Astronomical Society》2000,317(3):630-648
We present a study of numerical effects in dissipationless cosmological simulations. The numerical effects are evaluated and studied by comparing the results of a series of 643 -particle simulations of varying force resolution and number of time-steps, performed using three of the N -body techniques currently used for cosmological simulations: the Particle–Mesh (PM), the Adaptive Particle–Particle–Particle–Mesh (AP3 M) and the newer Adaptive Refinement Tree (ART) codes. This study can therefore be interesting both as an analysis of numerical effects and as a systematic comparison of different codes.
We find that the AP3 M and the ART codes produce similar results given that convergence is reached within the code type. We also find that numerical effects may affect the high-resolution simulations in ways that have not been discussed before. In particular, our study revealed the presence of two-body scattering, the effects of which can be greatly amplified by inaccuracies in time integration. This process appears to affect the correlation function of matter, the mass function, the inner density of dark matter haloes and other statistics at scales much larger than the force resolution, although different statistics may be affected in a different fashion. We discuss the conditions for which strong two-body scattering is possible and discuss the choice of the force resolution and integration time-step. Furthermore, we discuss recent claims that simulations with force softening smaller than the mean interparticle separation are not trustworthy and argue that this claim is incorrect in general, and applies only to the phase-sensitive statistics. Our conclusion is that, depending on the choice of mass and force resolution and the integration time-step, a force resolution as small as 0.01 of the mean interparticle separation can be justified. 相似文献
We find that the AP
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Andreas Faltenbacher rey V. Kravtsov Daisuke Nagai Stefan Gottlöber 《Monthly notices of the Royal Astronomical Society》2005,358(1):139-148
We study motions of galaxies in galaxy clusters formed in the concordance Λ cold dark matter cosmology. We use high-resolution cosmological simulations that follow the dynamics of dark matter and gas and include various physical processes critical for galaxy formation: gas cooling, heating and star formation. Analysing the motions of galaxies and the properties of intracluster gas in a sample of eight simulated clusters at z = 0, we study the velocity dispersion profiles of the dark matter, gas and galaxies. We measure the mean velocity of galaxy motions and gas sound speed as a function of radius and calculate the average Mach number of galaxy motions. The simulations show that galaxies, on average, move supersonically with the average Mach number of ≈1.4, approximately independent of the cluster-centric radius. The supersonic motions of galaxies may potentially provide an important source of heating for the intracluster gas by driving weak shocks and via dynamical friction, although these heating processes appear to be inefficient in our simulations. We also find that galaxies move slightly faster than the dark matter particles. The magnitude of the velocity bias, b v ≈ 1.1 , is, however, smaller than the bias estimated for subhaloes in dissipationless simulations. Interestingly, we find velocity bias in the tangential component of the velocity dispersion, but not in the radial component. Finally, we find significant random bulk motions of gas. The typical gas velocities are of order ≈20–30 per cent of the gas sound speed. These random motions provide about 10 per cent of the total pressure support in our simulated clusters. The non-thermal pressure support, if neglected, will bias measurements of the total mass in the hydrostatic analyses of the X-ray cluster observations. 相似文献