共查询到20条相似文献，搜索用时 62 毫秒
1.
针对任意各向异性地层,利用极向型和环向型标量位函数,导出相应的直流电视电阻率和磁电阻率的磁场响应关系.计算了各向异性地层的直流电视电阻率和磁电阻率响应特征,重点分析了电阻率测深方法与磁电阻率探测方法对地下各向异性介质的探测能力.文中采用状态矩阵的分析方法,首先采用极向型和环向型标量位构造了各向异性层状介质电场与磁场的通解,利用各层界面电场、磁场的连续性及地面激励源的耦合条件,推导了不同层之间电磁场的状态矩阵,建立了空间电场与磁场的递归计算关系.其次,针对递归计算中指数项数值计算的不稳定性,借用状态矩阵的性质,导出了将不稳定指数计算项转化为稳定的指数项的转换关系.针对横向各向同性(TI)介质中极向位与环向位解耦的特点,导出了电磁场的直接积分解.最后,采用解析解验证了算法的正确性,给出了多层各向异性地层模型的视电阻率和磁场响应曲线,分析了直流电法探测裂缝性地层、估计裂缝分布性状的可能性. 相似文献
2.
We study semi-analytical time-dependent solutions of the relativistic MHD equations for the fields and the fluid emerging from a spherical source. We assume uniform expansion of the field and the fluid and a polytropic relation between the density and the pressure of the fluid. The expansion velocity is small near the base but approaches the speed of light at the light sphere where the flux terminates. We find self-consistent solutions for the density and the magnetic flux. The details of the solution depend on the ratio of the toroidal and the poloidal magnetic field, the ratio of the energy carried by the fluid and the electromagnetic field and the maximum velocity it reaches. 相似文献
3.
It is one of the classical problems
in Earth′s electromagnetism that continuation of the observatory data of magnetic field
into the conducting region. This paper built the coupling vector equations governing the
poloidal, toroidal and potential fields in 3-D inhomogeneous conducting mantle.
Considering the limitation on variable scale of inhomogeneities in global mantle from
study of the Earth′s deep interior, a perturbation theory of gradually lateral
variation was presented. It is unnecessary that the 1-D spherical symmetric distribution
of electric conductivity as zero-degree approximation. Serving as a example of solvability
of the zero-degree approximation, it was demonstrated how the gradually lateral variation
of electric conductivity effect on anti-diffusive problem of poloidal field in Earth′s
mantel. 相似文献
4.
把磁场观测数据向导电区域延拓,是地球电磁学的经典问题之一．从准静态近似和非零矢势规范的电磁场方程出发,依据矢量的球面分解唯一性定理,本文建立支配三维非均匀电寻率分布全球地慢中的环型场、极型场和电位势场的耦合方程组烤虑地球深部研究对认识全球地幔非均匀性横向变化尺度的限制,提出横向缓变意义下三维非均匀地幔中电场和磁场的摄动理论,其零级近似不要求电导率分布一维球对称．作为零级近似可解的例证,研究了地幔深源极型场的反扩散问题,在利用地面磁场观测反演到核幔边界时,可以考虑地幄横向非均匀性影响． 相似文献
5.
The electrodynamic flare model is based on numerical 3D simulations with the real magnetic field of an active region. An energy
of ∼1032 erg necessary for a solar flare is shown to accumulate in the magnetic field of a coronal current sheet. The thermal X-ray
source in the corona results from plasma heating in the current sheet upon reconnection. The hard X-ray sources are located
on the solar surface at the loop foot-points. They are produced by the precipitation of electron beams accelerated in field-aligned
currents. Solar cosmic rays appear upon acceleration in the electric field along a singular magnetic X-type line. The generation
mechanism of the delayed cosmic-ray component is also discussed. 相似文献
6.
C. Narteau E. Blanter J. -L. Le Mouël M. Shirnman C. J. Allgre 《Physics of the Earth and Planetary Interiors》2000,120(4):271-287
We investigate the temporal evolution of the magnetic dipole field intensity of the Earth through a multiscale dynamo mechanism. On a large range of spatio-temporal scales, the helical motions of the fluid flow are given by a schematic model of a fully developed turbulence. The system construction is symmetric with respect to left-handed and right-handed cyclones. The multiscale cyclonic turbulence coupled with a differential rotation (schematic ω dynamo) or alone (schematic 2 dynamo) is the ingredient of the loop through which poloidal and toroidal fields are built from one another. Two kinds of reaction of the magnetic field on the flow are considered: the presence of a magnetic field first favours a larger-scale organization of the flow, and, second, impedes this flow by the effect of growing Lorentz forces. We obtain the general features of the geomagnetic field intensity observed over geological times and describe a general mechanism for reversals, excursions and secular variation. The mechanism happens to keep a memory during the chrons and loose it during the events (excursions and inversions). 相似文献
7.
A kinetic theory is necessary to explain the electron flows forming strong field-aligned currents in the auroral region. Its construction in this paper is based on the following propositions. (a) In the equatorial region, the arrival of electrons through the lateral surface of the magnetic flux tube is compensated for by their escape along the magnetic field. This is provided by action of the pitch-angle diffusion mechanism in the presence of plasma turbulence concentrated in this region. (b) Outside the equatorial region, the distribution functions of trapped and precipitating particles become “frozen.” The distributions and particle concentrations are calculated there in a model with conservation of the total energy and the magnetic moment. (c) The quasi-neutrality condition yields a large-scale parallel electric field, which contributes to the conserved total energy. In this field, the electron acceleration occurs, causing strong field-aligned currents directed upward from the ionosphere. 相似文献
8.
Willem V.R. Malkus 《Physics of the Earth and Planetary Interiors》1979,20(2-4):181-184
The linear solvability conditions are found for any field of force leading to steady motion in a stratified rotating medium. A general solution for such motion is determined. For the Lorentz force, it is shown that a unique relation between all axisymmetric poloidal and toroidal magnetic fields is specified. A path to solutions for the non-linear -dynamo stability problem compatible with these constraints is outlined. 相似文献
9.
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． 相似文献
10.
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． 相似文献
11.
Louis Baker 《地球物理与天体物理流体动力学》2013,107(1):257-278
Abstract Models of a convectively driven hydromagnetic dynamo are constructed using a truncated modal expansion. The resulting nonlinear partial differential equations are integrated numerically. The results confirm that rotation is a necessary condition for effective dynamo action, and suggest that equipartition of kinetic and magnetic energies is qualitatively valid, and that toroidal field energies can be much larger than poloidal. 相似文献
12.
We investigate the dynamo underpinning of solar cycle precursor schemes based on direct or indirect measures of the solar surface magnetic field. We do so for various types of mean-field-like kinematic axisymmetric dynamo models, where amplitude fluctuations are driven by zero-mean stochastic forcing of the dynamo number controlling the strength of the poloidal source term. In all stochastically forced models considered, the surface poloidal magnetic field is found to have precursor value only if it feeds back into the dynamo loop, which suggests that accurate determination of the magnetic flux budget of the solar polar fields may hold the key to dynamo model-based cycle forecasting. 相似文献
13.
Abstract This paper presents the first attempt to examine the stability of a poloidal magnetic field in a rapidly rotating spherical shell of electrically conducting fluid. We find that a steady axisymmetric poloidal magnetic field loses its stability to a non-axisymmetric perturbation when the Elsasser number A based on the maximum strength of the field exceeds a value about 20. Comparing this with observed fields, we find that, for any reasonable estimates of the appropriate parameters in planetary interiors, our theory predicts that all planetary poloidal fields are stable, with the possible exception of Jupiter. The present study therefore provides strong support for the physical relevance of magnetic stability analysis to planetary dynamos. We find that the fluid motions driven by magnetic instabilities are characterized by a nearly two-dimensional columnar structure attempting to satisfy the Proudman-Taylor theorm. This suggests that the most rapidly growing perturbation arranges itself in such a way that the geostrophic condition is satisfied to leading order. A particularly interesting feature is that, for the most unstable mode, contours of the non-axisymmetric azimuthal flow are closely aligned with the basic axisymmetric poloidal magnetic field lines. As a result, the amplitude of the azimuthal component of the instability is smaller than or comparable with that of the poloidal component, in contrast with the instabilities generated by toroidal decay modes (Zhang and Fearn, 1994). It is shown, by examining the same system with and without fluid inertia, that fluid inertia plays a secondary role when the magnetic Taylor number Tm ? 105. We find that the direction of propagation of hydromagnetic waves driven by the instability is influenced strongly by the size of the inner core. 相似文献
14.
Abstract Dynamic interaction between magnetic field and fluid motion is studied through a numerical experiment of nonlinear three-dimensional magnetoconvection in a rapidly rotating spherical fluid shell to which a uniform magnetic field parallel to its spin axis is applied. The fluid shell is heated by internal heat sources to maintain thermal convection. The mean value of the magnetic Reynolds number in the fluid shell is 22.4 and 10 pairs of axially aligned vortex rolls are stably developed. We found that confinement of magnetic flux into anti-cyclonic vortex rolls was crucial on an abrupt change of the mode of magnetoconvection which occurred at Δ = 1 ～ 2, where A is the Elsasser number. After the mode change, the fluid shell can store a large amount of magnetic flux in itself by changing its convection style, and the magnetostrophic balance among the Coriolis, Lorentz and pressure forces is established. Furthermore, the toroidal/poloidal ratio of the induced magnetic energy becomes less than unity, and the magnetized anti-cyclones are enlarged due to the effect of the magnetic force. Using these key ideas, we investigated the causes of the mode change of magnetoconvection. Considering relatively large magnetic Reynolds number and a rapid rotation rate of this model, we believe that these basic ideas used to interpret the present numerical experiment can be applied to the dynamics in the Earth's and other planetary cores. 相似文献
15.
The dynamics of stably stratified stellar radiative zones is of considerable interest due to the availability of increasingly detailed observations of Solar and stellar interiors. This article reports the first non-axisymmetric and time-dependent simulations of flows of anelastic fluids driven by baroclinic torques in stably stratified rotating spherical shells – a system serving as an elemental model of a stellar radiative zone. With increasing baroclinicity a sequence of bifurcations from simpler to more complex flows is found in which some of the available symmetries of the problem are broken subsequently. The poloidal component of the flow grows relative to the dominant toroidal component with increasing baroclinicity. The possibility of magnetic field generation thus arises and this paper proceeds to provide some indications for self-sustained dynamo action in baroclinically-driven flows. We speculate that magnetic fields in stably stratified stellar interiors are thus not necessarily of fossil origin as it is often assumed. 相似文献
16.
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18.
R.S. Peckover 《Physics of the Earth and Planetary Interiors》1973,7(2):137-142
In addition to the electric potentials induced by the gyral motions in the oceans, horizontal electric fields and currents result from the exchange of water between the depths and the surface in the presence of the main geomagnetic field. In this note a simple model representing such a circulation is considered, and the spatial distribution of the corresponding induced electric fields is calculated. A surface velocity of 2 knots could induce electric currents up to 10?4 Amp/m2. These steady currents in the ocean could be comparable with the normal oceanic daily variation. Since a proportion of the electric current would return through the earth below the sea floor, this calculation provides an upper limit to this component. An indication is also given of the magnetic field distortion and associated electric currents which occur in a highly conducting (Jovian) ocean. 相似文献
19.
Large-scale galactic magnetic fields are probably caused by some magnetic field amplification mechanism starting from a seed field. This seed field is still enigmatic. In this contribution it is shown that macroscopic sheared relative velocities of the charged and neutral components of a protogalactic partially ionized plasma generate magnetic fields during the protogalactic collapse. Plasma-neutral gas fluid simulations are performed in order to illustrate this magnetic field-self generation mechanism. 相似文献
20.
M.R.E. Proctor 《地球物理与天体物理流体动力学》2013,107(3):235-240
The well-known “toroidal theorem” of Elsasser and Bullard and Gellman rules out dynamo action in a conducting sphere when the velocity field has no poloidal part. It is here shown that for a fixed toroidal velocity field any poloidal velocity must attain a finite size if dynamo action is to be possible. The resulting “anti-dynamo” theorem generalises the earlier result of Childress by giving a bound on the product of the suprema of the toroidal and poloidal velocities. 相似文献