Subduction, back-arc spreading and global mantle flow

The shapes and orientations of Benioff zones beneath island arcs, interpreted as marking the location of subducted lithosphere, provide the best presently available constraints on the global convective flow pattern associated with plate motions. This global flow influences the dynamics of subduction. Subduction zone phenomena therefore provide powerful tests for models of mantle flow. We compute global flow models which, while simple, include those features which are best constrained, namely the observed plate velocities, applied as boundary conditions, and the density contrasts given by thermal models of the lithosphere and subducted slabs. Two viscosity structures are used; for one, flow is confined to the upper mantle, while for the other, flow extends throughout the mantle.Instantaneous flow velocity vectors match observed Benioff zone dips and shapes for the model which allows mantle-wide flow but not for the upper mantle model, which has a highly contorted flow pattern. The effect of trench migration on particle trajectories is calculated; it is not important if subduction velocities are greater than migration rates. Two-dimensional finite element models show that including a coherent high viscosity slab does not change these conclusions. A coherent high viscosity slab extending deep into the upper mantle would significantly slow subduction if flow were confined to the upper mantle. The maximum earthquake magnitude, M_w, for island arcs correlates well with the age of the subducted slab and pressure gradient between the trench and back-arc region for the whole mantle, but not the upper mantle, flow model. The correlations with orientations of Benioff zones and seismic coupling strongly suggest that the global return flow associated with plate motions extends below 700 km. For both models, regions of back-arc spreading have asthenospheric shear pulling the back-arc toward the trench; regions without back-arc spreading have the opposite sense of shear, suggesting global flow strongly influences back-arc spreading.     

On the possibility of Newtonian flow in the upper mantle

The possibility of a linear-creep (Newtonian-viscosity) upper mantle is reexamined on the basis of present knowledge on flow mechanisms in olivine, including differences between activation parameters for creep and for diffusion, and revised estimates of grain boundary width. Results of the comparison between linear superplastic creep and power-law creep are presented as crossover temperature between lattice and grain-boundary diffusion, and crossover stress between non-linear and linear creep, as a function of temperature (depth), grain size, grain-boundary width, grain-boundary diffusion activation energy, and rate-controlling species (silicon or oxygen). For the most realistic values of the parameters, linear creep is well within the range of possibilities. There is no major objection from rheology to the idea of a Newtonian-viscosity upper mantle.Viscosities for the two kinds of creep are compared for laboratory, upper mantle, and—tentatively—lower mantle conditions. This results in a prediction of the grain size at which Coble creep could be observed in olivine polycrystals in the laboratory (~ 10 μm or less). The upper mantle viscosity is in the 10²⁰–10²¹ Pa s range. Minimum estimates for the viscosity of the lower mantle are of the same order.The pictures of the rheology of the mantle derived from microphysical models of flow and from geophysical observation can therefore be made compatible.     

Possible orogeny-parallel lower crustal flow and thickening in the Central Andes

The relatively low elevation and thick crust in the Altiplano, in comparison to the higher elevation, but thinner crust in the Puna plateau, together with geophysical data, suggests that isostatic equillibrium is achieved by cooler and denser lithospheric mantle in the Altiplano. Excess density in the Altiplano mantle could create differential horizontal stress in the order of 25 MPa between both lithospheric columns. Numerical models accounting for pressure and temperature-dependent rheology show that such stress can induce horizontal ductile flow in the lower crust, from the Puna towards the Altiplano. With a minimum viscosity of 10¹⁹ Pa s, this flow reaches 1 cm/year, displacing more than 50 km of material within 5 Ma. If the lower crust viscosity is smaller, the amount of orogeny-parallel lower crustal flow can be even greater. Such a mechanism of channel flow may explain that different amounts of crustal material have been accommodated by shortening in the Altiplano and in the Puna. Because of the strength of the elastic-brittle upper crust, this channel flow does not necessitate large amounts of surface deformation (except vertical uplift), making it difficult to detect from the geology.     

根据汪清橄榄岩包体推导上地幔流变学状态初步研究

运用幔源橄榄岩包体的辉石地质温度计、地质压力计、橄榄石变形显微构造地质应力计以及橄榄石的高温流动律实验资料,计算上地幔的流变学参数是近年来探索上地幔流变学状态的一条新的途径,也是在地球物理手段之外研究上地幔状态的一个值得注意的进展^[1-4]。     

Slab–mantle flow interaction: influence on subduction dynamics and duration

We investigate the influence of mantle flow relative to the lithosphere on subduction dynamics. We use 2D thermo‐mechanical models assuming incompressible non‐Newtonian fluid rheology. Different mantle flow velocities consistent with absolute plate motion models are tested, as well as both directions of flow, either sustaining or opposing slab dip. The effects of different inflow/outflow velocity profiles, slab strengths and upper–lower mantle viscosity contrasts are also evaluated. Slab dip deviations between models with opposite mantle flow directions range from 37° for relatively strong slabs (η_max = 10²⁵ Pa s) to 50° for weaker slabs (η_max = 10²⁴ Pa s), accounting for a significant amount of natural slab dip variability. For imposed mantle flow supporting the slab, the initial stage of slab steepening is followed by a stage of continuous slab dip decrease. This slab shallowing eventually leads to mantle wedge closure, subduction cessation and slab break‐off, possibly driving subduction flips.     

On mantle drag force for the formation of a next supercontinent as estimated from a numerical simulation model of global mantle convection

Three‐dimensional spherical mantle convection was simulated to predict future continental motion and investigate the driving force of continental motion. Results show that both the time required (≥300 Ma from the present) and the process for the next supercontinent formation are sensitive to the choice of critical rheological parameters for mantle dynamics, such as a viscosity contrast between the upper and lower mantles and a yield strength of the lithosphere. From all the numerical models studied herein, mantle drag force by horizontal mantle flow beneath the continents may mostly act as a resistance force for the continental motion in the process of forming a new supercontinent. The maximum absolute magnitude of the tensional and compressional stress acting at the base of the moving continents is in the order of 100 MPa, which is comparable to a typical value of the slab pull force.     

Pressure dependence of melt viscosities on the join diopside-albite

The pressure dependence of melt viscosities on the join diopside-albite has been studied using falling-sphere viscometry. The five melt compositions investigated are: diopside, Ab₂₅Di₇₅, Ab₅₀Di₅₀, Ab₇₅Di₂₅ and albite. Experiments were performed at 1500° and 1600°C and at pressures of 5, 10, 15, 20 and 25 kbar. The positive and negative pressure dependence of the viscosity of diopside and albite, respectively, were confirmed. All intermediate compositions show an initial decrease in viscosity with increasing pressure; however, melt of Ab₂₅Di₇₅ composition passes through a minimum viscosity at approximately 12 kbar and 1600°C. This behavior is analogous to the variation in the viscosity of water with pressure at low temperature.

It is suggested that the three-dimensional, fully polymerized, albite structure dominates flow at low pressures. With increasing pressure, disruption of this structure and decrease in the average size of the flow units leads to domination by the diopside structure. The variation in viscosity with composition along the join at one atmosphere can be adequately modelled using the and (1965) configurational entropy model with an additional two-lattice configurational entropy of mixing term. The pressure dependence of viscosity in the diopside-albite system, however, cannot be predicted by the model, because there is an absence of information on the pressure dependence of the model parameters.

It is probable that relatively polymerized magmas (e.g. rhyolites to SiO₂-saturated basalts) show a negative pressure dependence of viscosity to depths where they originate in the lower crust or upper mantle. In contrast, the most depolymerized, naturally-occurring melts, such as strongly SiO₂-undersaturated basalts and picrites, may exhibit a viscosity minimum. The viscosity of these melts may be sufficiently high at depths within the upper mantle to inhibit their segregation, rise and eventual eruption at the surface.     

Buoyancy‐driven deformation and contemporary tectonic stress in the lithosphere beneath Central Italy

We studied the continental deformation and modelled the contemporary flow and stress distribution in the lithosphere beneath Central Italy. We made use of a revisited crust and uppermost mantle Earth structure that supports delamination processes. The model behaviour is primarily determined by the thick high density lithospheric root to the east and the low‐viscosity shallow mantle wedge to the west. The rate of the modeled crustal motion is in agreement with GPS data and the pattern of lithospheric flow explains the heat flux, the regional geology and provides a new background for the genesis and age of the recent Tuscan magmatism. The modelled stress in the lithosphere is spatially correlated with the prevailing stress field and the gravitational potential energy patterns and shows that buoyancy forces, solely, can explain the coexisting regional contraction and extension and the unusual sub‐crustal seismicity.     

Nature of the Moho Transition Zone in the Oman Ophiolite

The Moho Transition zone of ophiolites is dominantly composedof dunite, with various types of segregations (gabbros, pyroxenites,and chromitites). Representing a level of magmatic exchangebetween asthenospheric mantle and the constructing ocean crust,it records active melt circulation below a spreading ridge axisand offers the opportunity of observing the distribution ofmelt locally percolating and ponding in a deforming porous matrix.In the Oman ophiolite, the Moho Transition Zone has a thicknessvarying from ten to hundreds of meters; its thickness and compositionare related to the geometry of the asthenospheric mantle flow:thick Moho Transition Zones are on top of mantle diapirs characterizedby vertical flow, whereas thin Moho Transition Zones are presentin areas of horizontal mantle flow. A large high-temperatureplastic strain is recorded in thin Moho Transition zones, incontrast to thick ones where the strain is weaker and heterogeneous.Thick Moho Transition Zones display an intense magmatic activityexpressed by diffuse melt impregnations, dikes and sills. Inthese thick zones, we have studied the geometry of the meltcirculation at various scales. We present here the analysisof textures and lattice fabrics which record high-temperatureplastic strain and allow us to quantify it Melt circulates withinthe dunites and can locally destroy the solid framework, inrelation to a viscosity drop and the sharp overturn of mantleflow observed in this type of transition zone. KEY WORDS: Oman; ophiolite; Moho Transition Zone; textures ^*Corresponding author     

类地行星热物理条件与热演化影响因素分析——以火星地幔热柱演化为例

太阳系内类地行星具有相似的岩石层包围金属核的圈层结构,在行星幔的热演化历史起源方面具有同时性和同源性,并且都在早期变形重力位能加热的基础上随放射性热能衰减而冷却。但是,由于半径、密度、粘度以及表层构造属性等物理条件的差异,其热演化历史各具特色。依据基本的热对流和热传导方程,我们计算分析了类地行星热物理条件差异对行星幔热演化历史的影响。计算表明,类地行星热演化的早期,行星幔热对流是主要的散热方式。半径较大的行星表面热流密度大,平均散热量也大。半径较小的行星内部温差小,粘滞系数高,对流能力低,提早进入传导散热状态,且传导散热的岩石层也比大行星厚。不同边界层热物理条件下,类地行星幔热演化历史会分别出现逐渐冷却的平稳式、包含热柱上涌的波动式、行星幔幕次翻转的周期式等特点不同的热演化过程。火星内部曾经存在的地幔热柱构造与火星地幔热动力学演化过程密切相关。我们从火星地幔热动力学演化模型出发,定量计算与地幔热柱构造演化相关的地幔热动力学演化特征,通过三维球壳数值模拟,研究了火星地幔热演化历史上可能存在的热柱活动造成的火星热演化历史的非单调变化,火星地幔对流环结构随时间的演变方式,以及与边界相关的地幔热柱对火星地形的影响。     

Simple features of mantle-wide convection and the interpretation of lower-mantle tomograms

Simple fluid dynamic constraints aid in the interpretation of lower mantle tomograms. The geothermal gradient away from slabs and plumes is subadiabatic between the upper (lithosphere) and lower (D″) boundary layers by ～400 K. Slabs widen proportionally with the square root of the viscosity as they sink through the lower mantle. The time scale for the persistence of slab graveyards at the base of the mantle is comparable to the time for plate motions to reorganize ～120–200 Myr. At most a few starting plume heads currently exist in the lower mantle. Tomographic inversions may include more sophisticated numerical-modeling versions of these constraints.     

西北太平洋边缘海热流特征研究

西北太平洋各边缘海及其相应俯冲系统受深部构造活动等地质条件的控制,热流变化较大。在收集整理该区域最新的热流数据基础上,重点探讨西北太平洋俯冲带热结构相关理论、边缘海大洋岩石圈热演化理论模型和局部高异常热流的影响因素,总结了西北太平洋边缘海热流所反映的地质意义。研究结果表明,在西北太平洋“沟-弧-海”体系中,从“沟”到“弧”再到“边缘海”,热流密度呈“低-高-较高”的变化趋势,弧后地区整体表现为“均一高热”特征;千岛海沟、日本海沟和琉球海沟热流密度值在30.0 mW/m²左右,而对应的岛弧值为其2~3倍。弧后热流大小受到汇聚型俯冲带热结构的影响,俯冲带脱水作用导致的弧后上地幔黏度变化,地震速度降低,岩石圈弹性厚度减薄,引起小尺度地幔对流,形成弧后“均一高热”的热状态。热流的时空分布与岩石圈年龄也有关,随着岩石圈年龄增大,地表热流密度值会随之降低,热流密度值大小和离散性与其形成时间大致呈负相关。鄂霍次克海形成时代(30~65 Ma)较早,其热流密度值(86.8 mW/m²)和离散性(标准差3.727)相对较低;冲绳海槽目前还处于扩张阶段,其热流密度值(139.0 mW/m²)和离散性(标准差7.001)较高。浅层的地下水循环、断裂活动,深层的地幔部分熔融岩浆活动、弧后小尺度地幔对流、俯冲带拐角流等对局部异常热流起到一定程度的控制作用。     

Lithospheric gravitational instability beneath the Southeast Carpathians

The Southeast corner of the Carpathians, known as the Vrancea region, is characterised by a cluster of strong seismicity to depths of about 200 km. The peculiar features of this seismicity make it a region of high geophysical interest. In this study we calculate the seismic strain-rate tensors for the period 1967–2007, and describe the variation of strain-rate with depth. The observed results are compared with strain-rates predicted by numerical experiments. We explore a new dynamical model for this region based on the idea of viscous flow of the lithospheric mantle permitting the development of local continental mantle downwelling beneath Vrancea, due to a Rayleigh–Taylor instability that has developed since the cessation of subduction at 11 Ma. The model simulations use a Lagrangean frame 3D finite-element algorithm solving the equations of conservation of mass and momentum for a spatially varying viscous creeping flow. The finite deformation calculations of the gravitational instability of the continental lithosphere demonstrate that the Rayleigh–Taylor mechanism can explain the present distribution of deformation within the downwelling lithosphere, both in terms of stress localisation and amplitude of strain-rates. The spatial extent of the high stress zone that corresponds to the seismically active zone is realistically represented when we assume that viscosity decreases by at least an order of magnitude across the lithosphere. The mantle downwelling is balanced by lithospheric thinning in an adjacent area which would correspond to the Transylvanian Basin. Crustal thickening is predicted above the downwelling structure and thinning beneath the basin.     

西藏东巧方辉橄榄岩的显微构造特征及其流变学意义

西藏东巧地区蛇绿岩套中橄榄岩是青藏高原出露的为数不多的地幔岩体之一, 对于揭示该地区的上地幔流变学特征具有重要意义.报道了该地区方辉橄榄岩中橄榄石的位错显微构造特征, 估算了上地幔流变学参数.显微构造研究表明, 东巧方辉橄榄岩发育残斑结构, 橄榄石中位错组态类型比较丰富, 包括自由位错、位错壁(包括宽阔型和紧密型)、位错弓弯和位错网, 表明橄榄石的主导变形机制可能为位错蠕变.该区地幔岩变形大致分为2个阶段: (1) 地幔缓慢塑性流动变形, 形成宽阔型位错壁; (2) 蛇绿岩侵位过程中的变形, 产生紧密型位错壁.根据2种位错壁估算的流动应力平均值分别为3 9.3MPa (宽阔型)和113.9MPa (紧密型), 计算结果获得东巧地区上地幔流动速率为1.13× 10-12 ~ 2.95× 10-11s-1, 有效粘度为4.44×1017~ 1.16×1019Pa°s, 这些参数为东巧地区上地幔物理特征提供了流变学的约束条件      

Rheology of the upper mantle: Inferences from peridotite xenoliths

Stress estimates as a function of depth are obtained for peridotite xenoliths from the upper mantle of three types of tectonic environments by applying revised recrystallizedgrain-size paleopiezometry and pyroxene thermobarometry. The general increase in grain size with depth and hence decrease in deviatoric stress, observed previously, is confirmed but reversals in these trends are now established and remain enigmatic. Stresses and temperatures obtained are combined with a representative creep-flow law to calculate strainrate and viscosity profiles that appear to be physically reasonable. Profiles for the highthermal-gradient rift/ridge environments show a complexity that is interpreted as.a rheological discontinuity resulting from the emplacement of asthenospheric diapirs during late stages of continental rifting. Profiles for broad continental extension zones (C.E.Z.), believed to be most representative of oceanic upper mantle, fluctuate between 50 and 80 km, with a general small increase in strain rate and decrease in viscosity with depth; deepest samples apparently come from the base of the lithosphere. Profiles for the infracratonic mantle of southern Africa show nearly a uniform increase in strain rate to values greater than 10⁻¹⁴/sec, and a decrease in viscosity to lower than 10²¹ poise, at a depth of 230 km. These profiles may transect the mechanically defined lithosphere—asthenosphere transition at about 200 km and, if so, there is no evidence for a mechanical discontinuity at the boundary. This observation, coupled with evidence that the sense of shear is homogeneous for all mantle profiles constructed, clearly favors a model whereby lithospheric plates are dragged by thermal convection of the asthenosphere below. Sea-floor spreading rates and relative plate-velocity estimates are consistent with this interpretation but do not independently permit a definitive choice between the two favored models advanced to explain the driving force for plate motions.     

Thermal Structure and Rheology of the Upper Mantle beneath Guangdong and Hainan Provinces, China

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Numerical modeling of mantle convection in 3D on the SEE-GRID-SCI infrastructure

The Numerical Modeling of Mantle Convection (NMMC3D) application is calculating mantle convection models in 3D Cartesian domain. Our main goal is to study the structure and the surface manifestation (topographic and geoid anomalies) of the mantle plumes. The parameter study support tools of the P-GRADE grid Portal give an effective possibility to make an systematic investigation of the parameters influencing the character of mantle plumes. In collaboration with the MTA SZTAKI Application Porting Centre the NMMC3D has been ported to the SEE-GRID-SCI infrastructure. The paper introduces the steps that were taken to enable NMMC3D application on gLite based grid infrastructure and some results of the calculations. The main parameters influencing the mantle convection are the Rayleigh-number and the viscosity distribution of the mantle. In this paper the effect of these parameters is investigated on the thermal structure and surface manifestations of mantle plumes.     

On the implications of the coupled evolution of the deep planetary interior and the presence of surface ocean water in hydrous mantle convection

We investigate the influence of the deep mantle water cycle incorporating dehydration reactions with subduction fluxes and degassing events on the thermal evolution of the Earth as a consequence of core–mantle thermal coupling. Since, in our numerical modeling, the mantle can have ocean masses ∼12 times larger than the present-day surface ocean, it seems that more than 13 ocean masses of water are at the maximum required within the planetary system overall to partition one ocean mass at the surface of the present-day Earth. This is caused by effects of water-dependent viscosity, which works at cooling down the mantle temperature significantly so that the water can be absorbed into the mantle transition zone and the uppermost lower mantle. This is a result similar to that without the effects of the thermal evolution of the Earth's core (Nakagawa et al., 2018). For the core's evolution, it seems to be expected for a partially molten state in the deep mantle over 2 billion years. Hence, the metal–silicate partitioning of hydrogen might have occurred at least 2 billion years ago. This suggests that the hydrogen generated from the phase transformation of hydrous-silicate-hosted water may have contributed to the partitioning of hydrogen into the metallic core, but it is still quite uncertain because the partitioning mechanism of hydrogen in metal–silicate partitioning is still controversial. In spite of many uncertainties for water circulation in the deep mantle, through this modeling investigation, it is possible to integrate the co-evolution of the deep planetary interior within that of the surface environment.     

Origin of high-velocity anomalies beneath the Siberian craton: A fingerprint of multistage magma underplating since the Neoarchean

Despite the violent eruption of the Siberian Traps at ~ 250 Ma, the Siberian craton has an extremely low heat flow (18–25 mW/m²) and a very thick lithosphere (300–350 km), which makes it an ideal place to study the influence of mantle plumes on the long-term stability of cratons. Compared with seismic velocities of rocks, the lower crust of the Siberian craton is composed mainly of mafic granulites and could be rather heterogeneous in composition. The very high V_p (> 7.2 km/s) in the lowermost crust can be fit by a mixture of garnet granulites, two-pyroxene granulites, and garnet gabbro due to magma underplating. The high-velocity anomaly in the upper mantle (V_p = 8.3-8.6 km/s) can be interpreted by a mixture of eclogites and garnet peridotites. Combined with the study of lower crustal and mantle xenoliths, we recognized multistage magma underplating at the crust-mantle boundary beneath the Siberian craton, including the Neoarchean growth and Paleoproterozoic assembly of the Siberian craton beneath the Markha terrane, the Proterozoic collision along the Sayan-Taimyr suture zone, and the Triassic Siberian Trap event beneath the central Tunguska basin. The Moho becomes a metamorphism boundary of mafic rocks between granulite facies and eclogite facies rather than a chemical boundary that separates the mafic lower crust from the ultramafic upper mantle. Therefore, multistage magma underplating since the Neoarchean will result in a seismic Moho shallower than the petrologic Moho. Such magmatism-induced compositional change and dehydration will increase viscosity of the lithospheric mantle, and finally trigger lithospheric thickening after mantle plume activity. Hence, mantle plumes are not the key factor for craton destruction.     

On thermochemical mantle plumes with an intermediate thermal power that erupt on the Earth’s surface

The relative plume thermal power Ka = N/N₁ is used (N is the thermal power transferred from the plume base to its conduit and N₁ is the thermal power transferred from the plume conduit into the surrounding mantle in the steady-state heat conduction regime). Thermochemical mantle plumes with small (Ka < 1.15) and intermediate (1.15 < Ka < 1.9) thermal powers are formed at the core–mantle boundary beneath cratons in the absence of horizontal free-convection mantle flows beneath them, or in the presence of weak horizontal mantle flows. Thermochemical plumes reach the Earth’s surface when their relative thermal power is Ka > 1.15. The thermal and hydrodynamical structure of the plume conduit ascending from the core–mantle interface to the level from which the magmatic melt erupts on the Earth’s surface is presented. The model of two-stage eruption of the melt from the plume conduit to the surface is considered. The critical height of the massif above the plume roof, at which the eruption conduit supplying magmatic melt to the surface forms, is determined. The volume of melt erupting through the eruption conduit to the surface is estimated. The dependence of depth Δx from which the melt is transported to the surface on the plume diameter for a kinematic viscosity of ν = 0.5–2 m²/s is presented. In the case when the value Δx is larger than the depth starting from which diamond is stable (150 km), the melt from the plume conduit can transport diamonds to the Earth’s surface. The melt flow in the eruption conduit is considered as a turbulent flow in a cylindrical duct. The velocity of the melt flow in the eruption conduit and the time for the melt to be transported to the surface from a depth of Δx = 150 km for a kinematic viscosity of the melt in the eruption conduit ν_v = 0.01–1 m²/s are determined. Tangential stress on the eruption conduit sidewall is estimated in cases of melt flow both in smooth and rough conduits.