共查询到19条相似文献，搜索用时 500 毫秒
1.
修改了England和Mckenzie的黏性薄层流变模型中控制大陆形变的连续性方程,将剥蚀作用对高原隆升演化的影响直接引入该方程,并考虑下伏地幔小尺度对流对增厚岩石层的搬离作用对高原隆升演化后期的影响,用有限差分法直接模拟青藏高原隆升过程. 数值模拟结果所显示的高原隆升演化过程与实际观测资料吻合较好,揭示了高原隆升演化过程的非平稳和多阶段的特性;同时还表明上地幔小尺度对流对岩石层底部的搬离作用可能是最近8Ma以来高原快速隆升的主导机制. 相似文献
2.
在小尺度地幔对流模型的基础上,建立了顾及岩石层与地幔耦合的地幔对流模型,考虑到岩石层对上地幔小尺度对流的弹性响应,将上地幔视为一均匀的等粘滞系数的牛顿粘滞流体,其对注能量来源于下地幔,用热流体动力学基本方程得到地上地幔对流在壳幔边界处的垂向应力作为弹性板弯曲方程的垂直加载,来耦合弹性岩石层和可流动地幔,推导了两者耦合下区域重力异常和上地幔小尺度对流的相关方程,用以反演上地幔小尺度对流场模式和岩石层底部拖力场格局,对比了有,无弹性岩石层影响的模型之间的差异,并对模型应用范围,特别要板块边界水平均造力可能产生的影响,作了进一步探讨。 相似文献
3.
用数值模拟方法模拟了增厚大陆岩石层热边界层被对流地幔剥离并为软流层物质替代的动力学过程．结果表明,在初始温度分层分布、侧向均匀但存在微小热扰动的流场中,80km厚的增厚岩石层热边界层约需60Ma才能被完全剥离,剥离的速率微弱地依赖扰动的强度;在已建立好的流场中,同样厚度的增厚热边界层只需约10Ma就可被剥离．模拟结果暗示青藏高原地壳及岩石层在岩石层增厚和剥离以前就很热,其下伏地馒中可能已存在建立好的上地幔小尺度对流系统,而该尺度的对流系统很可能是由特提斯海洋岩石圈俯冲和消减诱发的 相似文献
4.
金星表层年龄和构造活动特点表明其岩石层在最近的地质历史时期经历过广泛的更新.这种全球性的表层改造与其内部热演化历史进程密切相关.如果金星存在相变形成的上、下地幔，依据现今所了解的金星物理性质和参量化的热对流理论，并且考虑金星地幔相变边界层状态对对流的控制作用，我们计算了金星热演化历史.结果表明，金星的热演化历史是一种非单调的冷却过程，在这种非单调的热演化历史进程中，金星地幔会出现大体等周期的翻转.由于参数选取的不同，翻转时金星上、下地幔的温差随时间可能出现稳定变化、逐渐加强、逐渐减弱三种不同演化模式，目前尚不能确定实际金星热演化历史究竟是哪一种模式.金星地幔相变边界层的穿透对流可能是推动其表层岩石层全球性更新的关键，导致其表层火山活动和地表构造以大致500 Ma时间间隔更新和重造. 相似文献
5.
本文分别基于数值结果和地质学模型,在假定地球的上地幔存在稳定Rayleigh-Bénard对流的基础上,模拟了直径为10 km（陨石坑直径约180 km,以Chicxulub为例）和直径为100 km（陨石坑直径约1000 km）的小行星撞击对地球的上地幔对流格局的影响.本文将直径10 km小行星的撞击效果等效为热异常,将直径100 km小行星的撞击效果等效为热异常和速度异常（主要指陨石坑底部的回弹）的叠加.计算结果表明,当小行星的直径在10 km左右时,撞击对上地幔对流的影响十分微弱,热扰动时间仅2—3 Ma;而当小行星的直径达到100 km时,撞击就会对上地幔对流产生强烈影响.这时,对流从扰动到新的稳态有一定模式可循（依次为：调整、多个对流环、调整、稳定）,扰动的持续时间受黏度和撞击点位置影响,同时稳定后地幔热柱会向着撞击点的方向产生一定的位移. 相似文献
6.
7.
利用全球重力大地水准面异常、板块绝对运动及全球地震层析成像数据,计算了青藏高原-天山地区岩石层下部地幔大尺度对流格局以及此种尺度对流驱动下岩石层内应力场分布;同时,利用区域均衡重力异常数据反演青藏高原中、北部到天山地区上地幔小尺度对流模型．结果表明,大尺度的地幔物质运移过程可能驱动着中国大陆岩石层整体从西部以南北方向为主的运动转向东部地区以北东和南东方向的运动;而该区域上地幔小尺度上升流动支持了现代青藏高原和天山地区的抬升运动．提出和讨论了青藏高原隆升的“断离隆升-挤压隆升-对流隆升”三阶段模式,并探讨了大陆岩石层构造运动的地幔深部动力学背景． 相似文献
8.
热和组分密度异常共同驱动的动态金幔柱解析模式给出金幔柱在金幔中上升的历史．当金幔柱到达岩石层底时其头部的特征量是5个独立变量的函数：（1）金幔柱起源的深度;（2）金幔粘性系数;（3）源温度异常值;（4）源组分与热密度异常之比;（5）金幔柱的浮力通量．基于新的Mapellan数据,金星表面上有360多个冠状和类冠状构造已被发现,其中65％直径小于300km．这类小型冠状构造被认为是由具有下述特征的较小的金幔柱所形成：（1）最大直径小于300km;（2）当其头部到达岩石层底时,过剩温度足以产生部分熔融层,应高于150K;（3）被冠状构造下面的金幔柱带上来的总浮力有能力支撑冠状构造隆起的总质量．用这3个条件分析数值结果并约束金幔柱的源参数,根据本文的数值实验结果,金星上的小型冠状构造可能是起源于上金幔小于1000km深度的动态金幔柱形成的． 相似文献
9.
在大地热流密度分布的基础上，研究了塔里木盆地中库尔勒－若羌和阿克苏－叶城两条剖面岩石层热结构特征．由岩石层Ｐ波速度分布转换成生热率剖面，用二维数值模型获得了岩石层热结构和热状态特征．结果表明，塔里木盆地壳幔边界温度的高低与其埋深密切相关．居里等温面深度大，地幔热流密度较低．岩石层厚度变化与其新生代期间挠曲过程密切相关．在岩石层温度分布基础上，确定了深部脆－韧性过渡带深度和岩石层屈服强度，表明塔里木盆地岩石层相对较冷，且具有刚性的地球动力学特征． 相似文献
10.
多种驱动力作用下东亚大陆形变及应力场演化 总被引：7，自引：0，他引：7
将印度板块持续地向北推进、下伏地幔小尺度对流对增厚大陆岩石层的搬离作用以及剥蚀作用视为形成现今东亚大陆形变和应力场格局的主驱动力。在一梯形区域内，利用数值模拟的方法，研究了东亚大陆在不同的边界条件、不同的剥蚀率系数及不同的岩石力学参数条件下的形变及应力场格局。与现代空间大地测量技术 CGPS)以及利用地震观测得到的结果进行了对比。结果表明，本文模型预测的结果与上述的观测结果有较好的吻合，其西部地区比东部吻合得更好。说明控制东亚大陆西部形变和应力场基本格局的主驱动力，来源于印度板块对欧亚板块的碰撞、挤压，而对东部地区还应当考虑其与太平洋板块和菲律宾板块的相互作用。与此同时，下伏地幔小尺度对流对增厚大陆岩石层的搬离作用以及风化剥蚀对应力场的演化过程也不可忽视。 相似文献
11.
Sean C. Solomon 《Physics of the Earth and Planetary Interiors》1979,19(2):168-182
The cores of the terrestrial planets Earth, Moon, Mercury, Venus and Mars differ substantially in size and in history. Though no planet other than the Earth has a conclusively demonstrated core, the probable cores in Mercury and Mars and Earth's core show a decrease in relative core size with solar distance. The Moon does not fit this sequence and Venus may not. Core formation must have been early (prior to ～4 · 109 yr. ago) in the Earth, by virtue of the existence of ancient rock units and ancient paleomagnetism and from UPb partitioning arguments, and in Mercury, because the consequences of core infall would have included extensional tectonic features which are not observed even on Mercury's oldest terrain. If a small core exists in the Moon, still an open question, completion of core formation may be placed several hundred million years after the end of heavy bombardment on tectonic and thermal grounds. Core formation time on Mars is loosely constrained, but may have been substantially later than for the other terrestrial planets. The magnitude and extent of early heating to drive global differentiation appear to have decreased with distance from the sun for at least the smaller bodies Mercury, Moon and Mars.Energy sources to maintain a molten state and to fuel convection and magnetic dynamos in the cores of the terrestrial planets include principally gravitational energy, heat of fusion, and long-lived radioactivity. The gravitational energy of core infall is quantifiable and substantial for all bodies but the Moon, but was likely spent too early in the history of most planets to prove a significant residual heat source to drive a present dynamo. The energy from inner core freezing in the Earth and in Mercury is at best marginally able to match even the conductive heat loss along an outer core adiabat. Radioactive decay in the core offers an attractive but unproven energy source to maintain core convection. 相似文献
12.
Patrick Cassen Ray T. Reynolds Frank Graziani Audrey Summers John McNellis Linda Blalock 《Physics of the Earth and Planetary Interiors》1979,19(2):183-196
The effect of solid convection on the thermal evolution of the Moon is explored for a variety of viscosities, radioactive differentiation efficiencies and initial temperature profiles. Convective heat flux in the models is calculated using an empirical relation derived from the results of laboratory experiments and numerical solutions of the Navier-Stokes equations. The method retains the spherically symmetric approximation and, therefore, greatly facilitates numerical calculations.Results show that even though solid convection may determine the thermal state of the lunar interior, it does not necessarily produce a quasi-steady thermal balance between heat sources and surface loss. An imbalance persists, due to the cooling and growth of the nonconvecting lithosphere. The state of the lithosphere is sensitive to the efficiency of heat source redistribution, while that of the convecting interior depends primarily on rheology. Convecting models have viscosities of 1021–1022 cm2s?1 in their interiors; the central temperature must be above 1100°C. Convection occurring within the first billion years after formation could have led to mare flooding by magma produced in hot zones of convection cells. However, it cannot be shown from model calculations alone that solid convection must have dominated lunar thermal history. 相似文献
13.
采用二维有限元数值模拟的方法研究了岩石圈的对流减薄过程,特别是克拉通岩石圈的对流减薄过程.模型的主要参数包括增厚岩石圈的宽度x、增厚倍数γ、以及与岩石圈组分变化导致的黏性和密度变化密切相关的黏性比(ηc)和浮力数(B)或等效密度变化(Δρtc).数值计算结果显示,地幔对流将逐渐减薄增厚的岩石圈部分,(1)当B=0和ηc=1时,即对一般地幔岩石圈,增厚岩石圈对流减薄的时间可表示为0.0073γ0.70 x0.26.将数值结果应用于地球,意味着增厚到300km的岩石圈,如宽度为300km,对流移除增厚部分回到初始平衡厚度120km大约需要225 Ma;如宽度为1500km,移除增厚部分大约需要342 Ma.(2)当B和ηc较小,克拉通岩石圈对流减薄过程与一般加厚岩石圈的对流减薄过程类似,但减薄时间受克拉通组分浮力和黏性比的影响而显著增长,克拉通岩石圈对流减薄的时间可表示为0.0057ηc0.52Δρ-0.21tcγ0.78ηc-0.36 x0.04.因而,对300km厚的克拉通岩石圈,如克拉通岩石圈的密度比周围地幔的密度低0.4%(即B=0.1),宽度1500km,若克拉通岩石圈黏性因组分影响比普通地幔岩石圈大10倍,其被对流减薄到120km大约需要1.18Ga.(3)当B和ηc增大到一定量时(如B≥0.2且ηc10),克拉通岩石圈被移除的过程将发生变化,由于组分浮力的影响,对流主要不是将克拉通岩石圈带到软流圈地幔中,而主要是将较厚的岩石圈物质向两边推送.在此情况下,克拉通岩石圈能长时间(3Ga)保持稳定. 相似文献
14.
SmNd isotopic data for mineral separates from the ferroan anorthosite 60025 define a precise isochron of 4.44 ± 0.02Ga age. This age is roughly 110 m.y. younger than the formation of the first large solid objects in the solar nebula, as recorded by the radiometric ages of the differentiated meteorites. In the magma ocean model for early lunar differentiation, ferroan anorthosites are the first crustal rocks to form on the Moon. If the Moon is as old as the oldest meteorites, the relatively young age determined for 60025 implies either that the magma ocean did not form synchronously with lunar formation, or that the magma ocean required over 100 m.y. before reaching the stage of ferroan anorthosite crystallization. Alternatively, we propose that the accumulated body of radiogenic isotope data for lunar rocks permit the Moon to be as young as 4.44–4.51 Ga. If so, isotopic evidence for chemical differentiation on the Earth at about this same time suggests that the formation of the Moon is reflected in the chemical evolution of the Earth. This, in turn, is consistent with the idea that the materials that now make up the Moon were derived from the Earth, perhaps ejected by collision between the Earth and another very large planetesimal during the final stages of accumulation of the terrestrial planets. Terrestrial origin models for the Moon lessen the requirement that the Earth and Moon each have near chondritic relative abundances of the refractory elements and could require that certain chemical and isotopic characteristics of both bodies be considered in the framework of the chemical mass-balance of the combined Earth-Moon system. 相似文献
15.
数值模拟华北克拉通岩石圈减薄的一种可能机制 ——下地壳榴辉岩重力失稳引起的拆沉 总被引：1，自引：1，他引：0
通过数值模拟研究,论证了中生代华北拉通岩石圈受挤压,下地壳玄武岩相变为密度较大的榴辉岩,榴辉岩重力失稳能够引起下地壳的拆沉,造成岩石圈的大规模减薄的可能性.通过对比不同规模的榴辉岩减薄方式发现,当榴辉岩规模较大时可能发生双管道拆沉,而规模小时发生单管道拆沉.计算结果表明当榴辉岩的水平尺度为100 km, 200 km, 300 km时,岩石圈拆沉减薄后厚度分别可达92 km,105 km,136 km.对比中生代华北克拉通岩石圈热侵蚀减薄和拆沉减薄机制,从力学机制上都能造成岩石圈减薄,但它们的结果对应着不同的地表地质特征.热对流减薄,中心区域变热变薄,中心区域是一个伸展区域,发展一个大的变质核杂岩区,岩浆的发展时序是从中心向两侧对称分布,并且向两侧减弱拆沉减薄结果中,中心区域受到挤压加厚,反而变冷.在中心区域的两侧发生两个减薄伸展区域,可能对应两个变质核杂岩区域,岩浆的发展时序是从两侧向中心减弱发展. 相似文献
16.
Hlne Rouby Marianne Greff-Lefftz Jean Besse 《Earth and Planetary Science Letters》2008,272(1-2):212-220
Motion of the entire solid planet with respect to its spin axis have been proposed on Mars. This movement is known as True Polar Wander (TPW). According to the conservation of angular momentum with no external torque, on geological time scales the axis of maximum inertia of a planet is aligned with the rotation axis. Then rearrangement of masses within the mantle disturbs the planet's inertia and induces TPW. The convection pattern on Mars is possibly controlled by a sequence of single plumes originating from the core-mantle boundary. Using a homogeneous model of the martian mantle and modelling the plume as a sphere, we calculate the inertial tensor perturbations caused by the plume mass anomaly. We investigate the stabilizing influence of the remnant rotational bulge due to the lithosphere elasticity on these perturbations. It appears that, during early martian history, the elastic lithosphere was thin enough to allow its fractures under the inertia perturbations induced by a hot plume. Consequently, the lithosphere's behaviour became effectively viscoelastic and the plume could induce large TPW. We conclude that one plume convection pattern should have greatly influenced the rotation pole behaviour during early Mars history: around 4 Gyr ago, Mars already could have experienced two TPW events lasting possibly only a few million years each. We then compare our scenario with others already published in the literature. 相似文献
17.
吕苗苗 《CT理论与应用研究》2019,28(2):175-186
青藏高原因其复杂的结构和演化历史,一直都是研究大陆碰撞、构造运动及其动力学的热点区域。本文采用三重震相波形拟合技术,基于中国地震观测台网和大型流动台阵记录到的某地震P波垂向记录,获得了包括拉萨、南羌塘和松潘甘孜地块在内的青藏高原上地幔P波速度结构。结果表明:①拉萨和南羌塘地块下方地幔过渡带存在高速异常,推测是俯冲的印度板片滞留体,过渡带底部的板片残余温度较低,使得660-km相变滞后约3～8km。而松潘甘孜地块下方过渡带同样存在高速异常,可能是欧亚岩石圈发生拆沉进入地幔过渡带所致。这说明印度板块俯冲作用的影响已经到达地幔过渡带,其俯冲前缘位于班公怒江缝合带附近。②从拉萨、南羌塘到松潘甘孜地块,200km之上的地幔岩石圈高速盖层速度由南向北逐渐减小,松潘甘孜地块则出现盖层缺失。推测受小规模地幔对流或者热不稳定性的影响,在南羌塘和松潘甘孜地块,增厚的欧亚岩石圈发生拆沉作用,岩石圈被减薄和弱化,造成羌塘地块上地幔低速和松潘甘孜地块上地幔高速盖层缺失。拆沉的冷的欧亚岩石圈可能部分停留在410-km上方,使得410-km抬升约10km,部分沉入地幔过渡带,表现为松潘甘孜地块地幔过渡带中存在高速异常。低温造成660-km下沉约8km,导致地幔过渡带增厚。 相似文献
18.
Since 1969, seismology has been extended beyond the Earth, and seismic sensors have been placed on the surface of other bodies of the solar system. A Lunar seismic network thus operated for the 8 years after 1969, with up to 4 stations, and detected some 1000 Moonquakes per year. A single seismic station was also operated on the Martian surface for 19 months since 1977. Unfortunately, it did not detect any Marsquakes, but produced useful information for future experiments. Remotesensing seismic experiments using Doppler shift observation have also been applied to Jupiter in the last two years and are beginning to return information on the normal modes. Planetary seismology is thus now well developed, and will provide increasing information on the structure and dynamics of the planets and bodies of the solar system. In this paper we review the state of the art in planetary seismology. For the terrestrial planets, we compare the seismic sources, structure and experiments on Earth, Moon and Mars. Such a comparison is useful in evaluating the design of past or future experiments. Results in the seismology of giant planets are also reviewed, stressing the connection between methods and theory. 相似文献
19.
The larger and most energetic cratering events from comet and asteroid collisions with the Earth are probably associated with ejection of solid material faster than escape speeds every 100 Myr or so. Metre-sized boulders, we estimate, may have been ejected directly into Venus-crossing and perhaps Mars-crossing orbits from comet impacts at higher speeds and of larger mass, at least on 10 occasions in the last 3.5 Ga. Subsequent close encounters with Earth can also enable slower boulders to reach Mars-crossing orbits. Orbit perturbations from Mars and Jupiter would then have sent a fraction of the boulders to the outer planets and their icy satellite systems. In the so-called late bombardment epoch at 3.9 Ga, when primitive life was developing, ejection-causing impacts were much more frequent, at 30 per 0.1 Ga, yielding an increased probability of distributing seeds of terrestrial biology to the outer regions of the solar system. 相似文献