Meridional circulation from differential rotation in an adiabatically stratified solar/stellar convection zone

Meridional circulation in stellar convection zones is not generally well observed, but may be critical for the workings of MHD dynamos operating in these domains. Coriolis forces from differential rotation play a large role in determining what the meridional circulation is. Here, we consider the question of whether a stellar differential rotation that is constant on cylinders concentric with the rotation axis can drive a meridional circulation. Conventional wisdom says that it can not. Using two related forms of the governing equations that respectively estimate the longitudinal components of the curl of the meridional mass flux and the vorticity, we show that such differential rotation will drive a meridional flow. This is because to satisfy anelastic mass conservation, non-spherically symmetric pressure contours must be present for all differential rotations, not just ones that depart from constancy on cylinders concentric with the rotation axis. Therefore, the fluid is always baroclinic if differential rotation is present. This is because, in anelastic systems, the perturbation pressure must satisfy a Poisson type equation, as well as an equation of state and a thermodynamic equation. We support our qualitative reasoning with numerical examples, and show that meridional circulation is sensitive to the magnitude and form of departures from rotation constant on cylinders. The effect should be present in 3D global anelastic convection simulations, particularly those for which the differential rotation driven by global convection is nearly cylindrical in profile. For solar-like differential rotation, Coriolis forces generally drive a two-celled circulation in each hemisphere, with a second, reversed flow at high latitudes. For solar like turbulent viscosities, the meridional circulation produced by Coriolis forces is much larger than observed on the Sun. Therefore, there must be at least one additional force, probably a buoyancy force, which opposes the meridional flow to bring its amplitude down to observed values.     

Mathematical Simulation of Convective Processes in the Liquid Core of the Earth and Implications for the Interpretation of Geomagnetic Field Variations in Polar Latitudes

The flow structure induced by thermal convection in a rotating spherical shell with viscous boundary conditions is considered under the assumption that the differential rotation of the core relative to the mantle is absent. The radial, azimuthal, and meridional components of the flow’s velocity and helicity are studied. With the magnetic field assumed to be frozen into a liquid (frozen-flux hypothesis), it is shown that the numerical results fit the observations of the geomagnetic field variations close to the pole.     

Convection in a rotating annulus having sidewalls of height-dependent thermal conductance

Abstract

Thermal convection in a vertically-mounted, rotating annulus of a particular design proposed by Davies and Walin (1977) is investigated. The annulus used in the present study differs from the conventional type in some important aspects: the sidewalls are finitely conducting, and the thermal conductance of the sidewalls is height-dependent. The theoretical model due to Davies and Walin is briefly recounted. The present study aims to verify the theoretical model; we have acquired numerical solutions to the governing Navier-Stokes equations. The numerical results are supportive of the theoretical contentions. The near-linear dependence of the isothermal slope on the parameter D, which is a function of Ω and ΔT, is corroborated within reasonable limits. New data on the vertical and radial structures of the meridional and azimuthal flows are presented. The numerical results also confirm that the shape of the sidewall thickness has a substantial influence on the meridional flow patterns. In the bulk of the interior flow field, the dominant azimuthal flow field and the temperature field are linked by the thermal wind relation.     

地幔对流与岩石层板块的相互耦合及影响──（Ⅱ）地幔混合对流理论及其应用

观测到的板块运动包含两种能量分布几乎相等的运动形态：极型场和环型场．纯粹的由热驱动的地幔自由对流不能预期和解释环型运动的产生．本文提出地幔混合对流理论，既考虑了热驱动的自由对流，也考虑了由板块自身激发的强迫对流．根据板块处于动力学平衡状态的观测事实，建立了相应的模型．数值结果表明，根据混合对流模型所预期的板块速度场，既能产生极型场，也能产生环型场，而且在空间分布特征及功率谱分布上与观测资料符合相当好．地幔物质的上升流动基本和洋脊对应，而下降流动和俯冲带对应．     

地幔对流与岩石层板块的相互耦合及影响──（Ⅱ）地幔混合对流理论及其应用

观测到的板块运动包含两种能量分布几乎相等的运动形态：极型场和环型场．纯粹的由热驱动的地幔自由对流不能预期和解释环型运动的产生．本文提出地幔混合对流理论，既考虑了热驱动的自由对流，也考虑了由板块自身激发的强迫对流．根据板块处于动力学平衡状态的观测事实，建立了相应的模型．数值结果表明，根据混合对流模型所预期的板块速度场，既能产生极型场，也能产生环型场，而且在空间分布特征及功率谱分布上与观测资料符合相当好．地幔物质的上升流动基本和洋脊对应，而下降流动和俯冲带对应．     

孟加拉湾西南季风与南海热带季风的气候特征比较

本文运用NCAR/NCEP再分析数据和APHRO_MA_V1003R1降水数据,对比分析了孟加拉湾西南季风和南海热带季风的气候特征异同以及对降水分布的影响,得到如下结论:(1)孟加拉湾西南季风比南海热带季风爆发更早、强度更强、持续时间更久、向北推进更北.(2)孟加拉湾西南季风建立过程缓慢,主要是索马里越赤道西南气流的逐渐加强和热带印度洋ITCZ(赤道辐合带)的逐渐北移;而南海热带季风建立过程迅速,主要是东亚大槽的一次替换过程伴随西太平洋副热带高压的突然东撤和热带西太平洋ITCZ的突然北跳.(3)孟加拉湾西南风纬向分量较强,季风建立前后主要变化在于偏西风的强度;而南海西南风经向分量较强,季风建立后风向突然逆转,东南风由于副高东撤而迅速被西南风取代.(4)孟加拉湾西南季风撤退较快,而南海季风则撤退较慢.(5)根据季风进程将夏季风期划分为季风发展期(5月)、强盛期(6-8月)和减退期(9-10月).其间对流活跃区的发展和推进、季风槽的位置以及对应降水区域均有明显差异.(6)在夏季风期,孟加拉湾和南海经度上分别存在着由ITCZ北抬引起的、在季风槽对流活跃区上升而在南北两侧下沉的、南北对称分布的季风经向次级环流.由于孟加拉湾和青藏高原强大热源的存在,孟加拉湾上升区南北跨度比南海的更大;孟加拉湾经圈环流更加稳定,而南海经圈环流的南北摆动更明显;孟加拉湾上升中心区比南海的偏北;在季风减退期,由于南海ITCZ撤退较慢,其上升区比孟加拉湾上升区偏北.     

Self-potential survey near the craters of Stromboli volcano (Italy). Inference for internal structure and eruption mechanism

The presence of self potentials on the upper part of Stromboli Volcano is associated with the existence of convection cells of gases and condensed liquids whose rising parts are situated above the hot zones. A model of a convection cell fed by a hot fluids through its lower middle part was calculated and applied to the various structures of the upper part of the volcano. This model which takes account of a process which is probably fairly common in volcanic system, gives a clear explanation of the various potential zones. Although other interpretations could be made, the fact that the positive and negative potentials are of the same importance, the limited size of the convection zone and the presence of gas under pressure beneath permeable grounds lead us to conclude that the phenomenological cause of these potentials is probably the mechanism of electro-filtration. The results of self-potential measurements showed very close correlation with those we obtained previously by magnetotelluric profiling. These two geophysical methods were very efficient in the precise delimitation of hot zones which give rise to resistivity and potential anomalies. The depth of those zones was estimated from the aspects of the potential anomalies and from the geological environment. The two methods were furthermore powerful tools in the investigation of volcanological processes and in particular the «Strombolian» rythmic eruption. The geometrical disposition of the feeding channels involves the obstruction of the path of the gases by the lava. Generally, the force of pressure exerted by the gas increases quickly and in consequence the plug of lava is ejected and shattered. When the gas flow lessens, the forces of viscosity increase quicker than the forces of pressure, the discharging outlets are then obstructed and thus there is great hazard that the accumulated energy will be liberated in a very violent fashion. In this case there will be a paroxysmal-type eruption. This mechanism is the consequence of a recent accident in the volcano evolution: the landslip of a segment of the cone, probably associated with the subsidence of the central caldera; the lava spread over the collapsed sector and the rhythmic eruptions described above constructed the present craters.     

Modeling of the solar activity double cycle using dynamical systems

The generation and evolution of the Sun’s magnetic field and other stars is usually related to the dynamo mechanism. This mechanism is based on the consideration of the joint influence of the α effect and differential rotation. Dynamo sources can be located at different depths of the convection zone and can have different intensities. Based on such a system, the dynamical system in the case of the stellar dynamo in a two-layer medium has been constructed with regard to meridional fluxes in order to model the double cycle that corresponds to the simultaneous presence of 22-year and quasi-biennial magnetic field oscillations. It has been indicated that the regime of mixed oscillations can originate because a dynamo wave moves oppositely to the meridional flows in the upper layer of the convection zone. This results in the deceleration of the toroidal field propagation and in the generation of slow oscillations. In deeper layers, the directions of a dynamo wave and meridional flows coincide with each other, as a result of which fast magnetic fields originate. Therefore, the total contribution of two oscillations with different frequencies corresponds to the appearance of quasi-biennial cycles against 22-year cycles. It has been indicated that the beating regime, which can be related to the secular oscillations of solar magnetic activity, originates in the system when the meridional flows are weak.     

热带大洋对纬向和经向风应力的联合响应

考虑了经向风应力和纬向风应力联合作用下热带大洋的响应问题.结果表明,只有一阶的经向风应力或具有辐合辐散的经向风应力才对最后的速度场和位势场造成影响.零阶的扰动温跃层和纬圈流受风应力的直接驱动和Kelvin波、Rossby短波的影响,而Rossby短波由经向风应力直接造成;二阶模则受风应力的直接驱动和Rossby短波的作用,同时经向风应力也产生了附加的Rossby短波.另外,在西边界处存在很强的暖水补充到赤道的现象,经向风应力有使暖水向赤道输送的作用,而西风应力使西边界处的暖水向东输送.     

Models of solar differential rotation

Abstract

Models of a differentially rotating compressible convection zone are calculated, considering the inertial forces in the poloidal components of the equations of motion. Two driving mechanisms have been considered: latitude dependent heat transport and anisotropic viscosity. In the former case a meridional circulation is induced initially which in turn generates differential rotation, whereas in the latter case differential rotation is directly driven by the anisotropic viscosity, and the meridional circulation is a secondary effect.

In the case of anisotropic viscosity the choice of boundary conditions has a big influence on the results: depending on whether or not the conditions of vanishing pressure perturbation are imposed at the bottom of the convection zone, one obtains differential rotation with a fast (≥ 10 ms^?1) or a slow (～ 1 ms^?1) circulation. In the latter case the rotation law is mainly a function of radius and the rotation rate increases inwards if the viscosity is larger in radial direction than in the horizontal directions.

The models with latitude dependent heat transport exhibit a strong dependence on the Prandtl number. For values of the Prandtl number less than 0.2 the pole-equator temperature difference and the surface velocity of the meridional circulation are compatible with observations. For sufficiently small values of the Prandtl number the convection zone becomes globally unstable like a layer of fluid for which the critical Rayleigh number is exceeded.     

青藏高原热状况和海温异常对亚洲季风季节转换年际变化的影响

本文根据季节转换前后副高脊面附近经向温度梯度变号的本质，利用相关分析和合成分析等方法研究了季节转换年际变化与外部影响因子的联系. 结果表明，冬春季青藏高原热状况和ENSO（El Nio/Southern Oscillation，厄尔尼诺/南方涛动）是决定亚洲季风区季节转换年际变化的主要因素. 当冬、春季海温呈现El Nio异常时，Walker环流减弱，于是西太平洋暖池区对流活动受到抑制，而赤道东太平洋对流活动加强则强迫赤道印度洋地区产生绝热下沉运动，使得印度洋地区大气偏暖，结果增大了南北向温度梯度，季节转换往往偏晚. 反之，季节转换偏早. 初春高原上空对流层中高层的气温异常对于判断季节转换迟早有很好的指示意义.     

Mantle flow with existence of plates and generation of the toroidal field

The observed plate velocities contain two types of motions. The poloidal component is related to the formation of ridges and subduction zones and the toroidal field expresses the shearing of surface plates. One very important consideration in modeling flow in the earth's mantle is the existence and motion of the lithospheric plates. The motion of plates represents a large-scale circulation with strong viscous coupling to the mantle underneath. The mantle flow probably is neither a purely free convection driven by buoyancy forces due to nonadiabatic temperature gradients in the mantle nor a forced convection generated by boundary forces, but a mixed convection that combines the effects of boundary and buoyancy forces. We present, in this paper, the mixed convection model resulting in a surface velocity field that contains both the observed poloidal and toroidal components.     

Convection in rotating annular channels heated from below. Part 1. Linear stability and weakly nonlinear mean flows

Convection in a Boussinesq fluid in an annular channel rotating about a vertical axis with lateral rigid sidewalls, stress-free top and bottom, uniformly heated from below is investigated. The sidewalls are assumed to be either perfectly insulating or conducting. Three different types of convection are identified when the channel is rotating sufficiently fast: (i) global oscillatory convection preferred for small Prandtl numbers in channels with intermediate or large aspect ratios (width to height ratio), (ii) wall-localized oscillatory convection representing the most unstable mode for moderate or large Prandtl numbers in channels with intermediate or large aspect ratios and (iii) global stationary convection preferred in channels with sufficiently small aspect ratios regardless of the size of the Prandtl number. The corresponding weakly nonlinear problem describing differential rotation and meridional circulation is also examined, showing that geostrophic, multiple-peaked (two prograde and two retrograde) differential rotation can be maintained by the Reynolds stresses in wall-localized convective eddies in a rapidly rotating channel.     

从经向气流看亚澳季风的季节区域特征

利用1979～2003年的NCEP/NCAR再分析资料探讨了亚澳季风区经向气流的季节性分支和结构特征. 结果表明,亚澳季风区经向气流的垂直斜压结构由冬到夏发生季节性转向,即从冬季时的低层北风、高层南风转换为夏季时的低层南风、高层北风. 季节反向的经向气流主体偏向北半球,其区域差异性在对流层中低层更为显著. 以印度半岛和中南半岛为界,亚洲热带季风区中低层经向气流在冬夏季均呈现三通道特征,与此相应,亚澳季风区自西向东存在三支相对独立的经向环流分支,且冬夏季的差异均很显著,如冬季的中心高度自西向东递减、夏季的经向跨度自西向东递增等.     

中国东部西南低空急流日变化特征及其机制

本文利用Final Global Data Assimilation System (FNL) 6小时再分析数据集分析了西南低空急流的日变化特征及其影响因子,结果表明:西南低空急流具有明显的日变化特征,在夜间和早晨(02LST,08LST)中国东南大部分地区急流发生频率较高,而在白天和傍晚(14LST,20LST)低空急流发生频率较低.经向地转风分量在一天内基本保持稳定,经向非地转分量在02LST最强,占实际风场强度50%以上,而在14LST和20LST,经向风场近似满足地转平衡.对风场非定常性、风速在流动方向上的非均匀性、流线弯曲和大气斜压性产生的地转偏差的分析结果表明,经向非地转风的日变化主要是由局地变压、水平风场涡度、垂直运动和温度梯度的日变化产生,副热带高压强度和位置的变化、青藏高原大地形加热效应和昼夜间海陆热力性质差异是造成经向非地转风夜间加强的重要原因.在中国东部地区,风速在流动方向的非均匀性虽然有利于非地转风的产生,但其没有明显的日变化,不是经向非地转风在夜间加强的主要原因.     

On formation of the intermediate water in the Northern Pacific Ocean

Summary Meridional cross sections of temperature, salinity and oxygen of the North Pacific Ocean are prepared to show location of the intermediate water, which is formed at the polar front and spreads on constantsigma-t surfaces. Geostrophic flow in a meridional plane is obtained by dynamic calculation. Friction-driven meridional circulation is determined from the zonally averaged density distribution. The latter flow seems to be more appropriate for explanation of mechanism of spread of the water.Oceanographic Institute Contribution No. 174.     

全球地幔垂直流动速度研究

用高分辨率地震体波速度成像以及相关的地球物理资料,计算地幔垂直流动形式及流动速度,得到全球地幔流垂直运动模式.从全球尺度来看,地幔流基本可划分为以下几个区域：欧亚大陆—澳大利亚、北美洲—南美洲为两个大规模下降流区域,西印度洋—非洲及大西洋、中南太平洋及东太平洋为两个大规模地幔上升流区域.地幔上升流起源于核幔边界,主要表现在地幔中部和上地幔下部.地幔垂直流动速度约每年1～4cm.地幔流动对地表板块运动、海洋中脊和中隆、俯冲带和碰撞带的分布起着控制作用.地幔上升流与地表现代热点有密切关系.从东亚尺度看,地幔流大体分为三个区域：东亚边缘裂谷系和西太平洋边缘海为上升流、西伯利亚地幔深度表现为物质下降流、青藏高原—缅甸—印度尼西亚特提斯俯冲带地幔下降流,这三个区域地幔流动与地表的西太平洋构造域、亚洲构造域和特提斯构造域相吻合.勾勒出南海地区构造特征：从上到下的大体结构是上部呈“工"字型、中间为圆柱型、底部呈盾形的地幔上升流.     

Convection in a rotating cylinder with its sidewall having a finite thermal conductance

Abstract

An investigation is made of steady thermal convection of a Boussinesq fluid confined in a vertically-mounted rotating cylinder. The top and bottom endwall disks are thermal conductors at temperatures T_t and T_b with δT = T_t ? T_b >0. The vertical sidewall has a finite thermal conductance. A Newtonian heat flux condition is adopted at the sidewall. The Rayleigh number of the fluid system is large to render a boundary layer-type flow. Finite-difference numerical solutions to the full Navier-Stokes equations are obtained. The vertical motions within the buoyancy layer along the sidewall induce weak meridional flows in the interior. Because of the Coriolis acceleration, the meridional flows give rise to azimuthal flows relative to the rotating container. Strong vertical gradients of azimuthal flows exist in the regions near the endwalls. As the stratification effect increases, concentration of flow gradients in thin endwall boundary layers becomes more pronounced. The azimuthal flow field exhibits considerable horizontal gradients. The temperature field develops horizontal variations superposed on the dominant vertical distribution. As either the sidewall thermal conductance or the stratification effect decreases, the temperature distribution tends to the profile varying linearly with height. Comparisons of the sizes of the dynamic effects demonstrate that, in the bulk of flow field, the vertical shear of azimuthal velocity is supported by the horizontal temperature gradient, resulting in a thermal-wind relation.     

Can zonally symmetric inertial waves drive an oscillating zonal mean flow?

In the present paper zonal mean flow excitation by inertial waves is studied in analogy to mean flow excitation by gravity waves that plays an important role for the quasi-biennial oscillation in the equatorial atmosphere. In geophysical flows that are stratified and rotating, pure gravity and inertial waves correspond to the two limiting cases: gravity waves neglect rotation, inertial waves neglect stratification. The former are more relevant for fluids like the atmosphere, where stratification is dominant, the latter for the deep oceans or planet cores, where rotation dominates. In the present study a hierarchy of simple analytical and numerical models of zonally symmetric inertial wave-mean flow interactions is considered and the results are compared with data from a laboratory experiment. The main findings can be summarised as follows: (i) when the waves are decoupled from the mean flow they just drive a retrograde (eastward) zonal mean flow, independent of the sign of the meridional phase speed; (ii) when coupling is present and the zonal mean flow is assumed to be steady, the waves can drive vertically alternating jets, but still, in contrast to the gravity wave case, the structure is independent of the sign of the meridional phase speed; (iii) when coupling is present and time-dependent zonal mean flows are considered the waves can drive vertically and temporarily oscillating mean flows. The comparison with laboratory data from a rotating annulus experiment shows a qualitative agreement. It appears that the experiment captures the basic elements of the inertial wave mean flow coupling. The results might be relevant to understand how the Equatorial Deep Jets can be maintained against dissipation, a process currently discussed controversially.     

Effect of the oceanic lithosphere velocity on free convection in the asthenosphere beneath mid-ocean ridges

The paper presents results obtained in experiments on a horizontal layer heated from below in its central part and cooled from above; the layer models the oceanic asthenosphere. Flow velocity and temperature profiles are measured and the flow structure under boundary layer conditions is determined (at Rayleigh numbers Ra > 5 × 10⁵). The flow in the core of a plane horizontal layer heated laterally and cooled from above develops under conditions of a constant temperature gradient averaged over the layer thickness. The flow core is modeled by a horizontal layer with a moving upper boundary and with adiabatic bounding surfaces under conditions of a constant horizontal gradient of temperature. Exact solutions of free convection equations are found for this model in the Boussinesq approximation. Model results are compared with experimental data. Temperature and flow velocity ranges are determined for the boundary layer regime. Based on the experimental flow velocity profiles, an expression is found for the flow velocity profile in a horizontal layer with a mobile upper boundary heated laterally and cooled from above. Free convection velocity profiles are obtained for the asthenosphere beneath a mid-ocean ridge (MOR) with a mobile lithosphere. An expression is obtained for the tangential stress at the top of the asthenosphere beneath an MOR and the total friction force produced by the asthenospheric flow at the asthenosphere-lithosphere boundary is determined.