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solar dynamo
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  太阳发电机
     In this paper, the two-scale analytical method of mean field electrodynamics and some research results, such as α, β effects and α2, α-w solar dynamo models, are reviewed.
     本文介绍了太阳湍流发电机问题的双尺度平均场电动力学分析方法以及有关太阳发电机问题的研究结果:α,β效应及各种发电机模型。
短句来源
     Progress in Solar Dynamo Theories
     太阳发电机理论研究进展
短句来源
     The main difficulties both in observation and in theory are pinpointed, and the other solar dynamo models are briefly described.
     总结分析了现阶段太阳湍流发电机问题在观测和理论方面的主要困难。 对其他的太阳发电机理论也进行了简要介绍。
短句来源
     Some results of a new nonlinear three-dimensional solar dynamo model are also presented.
     本文也给出了一个新的非线性三维太阳发电机模型。
短句来源
     The solar dynamo, which explains the origin and the evolution of all magnetic fields observed on the sun, is the fundamental and essential question of Solar Physics.
     太阳发电机理论主要解释太阳磁场的起源和演化,是太阳物理中最基本、最重要的问题之一。
短句来源
  “solar dynamo”译为未确定词的双语例句
     In comparison with typical solar spots, three distinct features of starspots, huge area, long life-time and the possibility for them to emerge in polar region, have given a striking challenge to the solar dynamo theory.
     对已取得的有关恒星黑子的观测分析结果作了概括,与太阳典型黑子情况作了对比,并对恒星黑子的巨黑子、极区黑子以及长寿命黑子特殊性作了讨论。
短句来源
     With the development of helioseismology, the solar dynamo has made great progresses.
     随着日震学的发展,该理论也得到了很大改进。
短句来源
     A relic field can help us to explain many asymmetries in solar activities, such as the north-south asymmetries of solar magnetic activities, active longitudes and holes, low-latitude coronal holes, Maunder minimum, etc. In addition it can affect the distribution and evolution of solar surface magnetic field by changing the boundary conditions of solar dynamo.
     太阳剩余磁场的存在不仅能够解释太阳活动的很多不对称性现象,如南北不对称性、活动经度与活动穴、低纬度冕洞和Maunder极小期等,还能通过改变自激发发电机模型的边值条件而影响整个太阳表面磁场的分布与演化。
短句来源
  相似匹配句对
     Progress in Solar Dynamo Theories
     太阳发电机理论研究进展
短句来源
     THE CURRENT STATUS OF SOLAR TURBULENT DYNAMO
     关于太阳湍流发电机理论
短句来源
     SOLAR STILLS
     太阳能蒸馏器
短句来源
     Solar sail
     太阳帆推进
短句来源
     APPROACH TO DYNAMO THEORY
     对发电机机制理论的近似(英文)
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  solar dynamo
As a result, it is still uncertain where and how the solar dynamo operates.
      
(I)CMEs are multi-dimensional, multi-parameter, and multi-scale phenomena related to the solar dynamo, corona, and heliosphere.
      
Planetary influences are ruled out; the variability is intrinsic and is described by the solar dynamo.
      
In this paper we demonstrate that resonance may play a crucial role in the dynamics of the climate system, by using the output from a nonlinear solar dynamo model as a weak input to a simplified climate model.
      
A key feature of this procedure is that the original time series is first transformed into a symmetrical space where the dynamics of the solar dynamo are unfolded in a better way, thus improving the model.
      
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The magnetic fluid in the solar convection zone tends to be driven to float by the magnetic buoyancy of the toroidal magnetic field, which is produced by the ω-effect of the solar dynamo. Consequently, phenomena of active regions in bipolar magnetic fields of sunspots will be formed on the surface of the sun.We see that the dimension of a buoyant magnetic fluid-mass which produces bipolar sunspots, may be large enough as to be comparable to the supergranulation, and meanwhile, that turbulence in this mass...

The magnetic fluid in the solar convection zone tends to be driven to float by the magnetic buoyancy of the toroidal magnetic field, which is produced by the ω-effect of the solar dynamo. Consequently, phenomena of active regions in bipolar magnetic fields of sunspots will be formed on the surface of the sun.We see that the dimension of a buoyant magnetic fluid-mass which produces bipolar sunspots, may be large enough as to be comparable to the supergranulation, and meanwhile, that turbulence in this mass may probably exist as indicated by the decaying time of sunspot magnetic fields. Therefore, it is possible for us to describe the buoyant process of a magnetic fluid-mass as a motion of mean flow. Since a solar radial gradient of turbulent magnetic diffusivity is there in the solar convection zone (Stix, 1976, Fig. 1), the difference of turbulent magnetic diffusivity across the boundary of the fluid mass will grow up with the increasing height of elevation. Thus, a large gradient of turbulent magnetic diffusivity comes to exist at the boundary of this mass during it striving its way up.Generally speaking, the elevating magnetic fluid will form an irregularly shaped fluid mass of convective material. Our purpose is only to study the magnetic characteristics at the boundary of the fluid mass when it traversed the toroidal field. Therefore, we discuss merely an idealized model of spherical fluid mass with average radius γ0 and equilibrium elevating velocity vc, neglecting other fine characteristics of irregular shaping of the mass and its possible inner circulations etc.The magnetic Reynolds number of the elevating process for a fluid mass is Rm=vcγ0/η, here η is the turbulent magnetic diffusivity. Our result is for the motion with small magnetic Reynolds number, Rm<1. We have noticed from the well-known induction equation that the toroidal magnetic field is to be disturbed by the striking gradient of the turbulent magnetic diffusivity across the boundary of the fluid mass after its passing over. We develop the induction equation in the coordinate system moving with the elevating fluid mass. Taking the total magnetic field as B', we have B' = B* + B, here B* is the toroidal magnetic field and B is the additional magnetic field induced by the disturbance of the fluid mass. Substituting B'=B* + it into the induction equation, we get equation (3.5) which describes the magnetic field B. By use of the condition of cylindrical symmetry in this problem, we solve equation ' (3.5) finally to achieve formula (3.22). It is clearly shown that a magnetic flux ring has formed around the surface of the fluid mass (Pig. 4). The final result is that two oppositely polarized magnetic regions will emerge on the surface of the sun as the magnetic ring is brought to the top of solar convection zone by the elevating fluid mass. According to this reason, we attempt to explain the phenomena why the bipolar magnetic fields of sunspots are concentrated in small bundles of high field strength. By means of the characteristics of the magnetic ring and toroidal magnetic field, other characteristics of bipolar magnetic field of sunspots may also be explained extensively.''

在太阳对流层内,由于ω-效应产生了很强的纬向磁场,它的磁浮力引起了磁流体的上浮,在太阳表面造成了黑子双极磁场等活动区的现象。本文考虑了在磁流团上浮后,由于在太阳对流层内存在湍流磁扩散率的垂直梯度,因而在磁流团内外的磁扩散率之差要随磁流团上升距离的增加而增大,以致在磁流团表面形成了巨大的磁扩散率的梯度,从磁感应方程中可以看到,这一梯度将扰动纬向磁场,结果在磁流团表面形成了磁环,它随磁流团浮升到对流层顶,在太阳表面呈现出两个极性相反的磁区。本文企图以此来说明黑子双极磁场密集性原因的尝试。

According to the ω-effect of the solar dynamo theory, a very strong toroidal magnetic field is produced in the solar convection zone. The fluid mass in the solar convection zone tends to rise by the magnetic buoyancy of the toroidal magnetic field. We discussed, in the paper [5] , that the gradient of the magnetic diffusivity on the surface of rising fluid mass must have disturbed the toroidal, magnetic field. This disturbance attempts to concentrate toroidal magnetic field on the surface of...

According to the ω-effect of the solar dynamo theory, a very strong toroidal magnetic field is produced in the solar convection zone. The fluid mass in the solar convection zone tends to rise by the magnetic buoyancy of the toroidal magnetic field. We discussed, in the paper [5] , that the gradient of the magnetic diffusivity on the surface of rising fluid mass must have disturbed the toroidal, magnetic field. This disturbance attempts to concentrate toroidal magnetic field on the surface of fluid mass because there is a large gradient of magnetic diffusivity on its surface, thus a sunspot magnetic flux ring is formed around the surface of, the fluid mass.The instability in the development of sunspot magnetic ring in the disturbance as mentioned above is further studied with the hydromagnetic perturbation equations in this paper. We get the conclusion that there is an instable mode in the perturbation equations. The reason of this instability is as follows: When the temperature (equiv. magnetic diffusivity et seq.) is disturbed in somewhere, the toroidal magnetic field will be disturbed and concentrated at that place where there is a large gradient of temperature. This concentrating of the toroidal magnetic field causes an increase in magnetic pressure and a decrease in gas pressure which consequentially induces a decrease in temperature and an increase in the gradient of temperature with the adiabatic process. The increased gradient of temperature results a further concentration of toroidal magnetic field. The relationship of mutual promoting between the magnetic field and the temperature is now called magnetic diffusion instability.

根据太阳发电机理论中的ω-效应,在太阳对流层内将产生纬向磁场,它的磁浮力要促使流团上浮。在文[5]中讨论了在流团上浮过程中,流团表面的磁扩散率梯度将对纬向磁场产生扰动,这一扰动使纬向磁场集积在流团表面磁扩散率梯度大的地方,围绕流团表面形成了黑子磁环。 本文进一步从磁流力学方程组的小扰动方程出发探讨了太阳黑子磁环发展的不稳定性问题。结果表明:在扰动方程中存在着不稳定模式。这一不稳定性产生的原因是由于当温度(或者说磁扩散率)受到小扰动时,纬向磁场要集积在磁扩散率(或温度)梯度大的地方,而磁场的集积将导致磁压增强及气压减低。在绝热条件下,这将使温度减低,而温度的减低又加强了温度梯度的增大,这又进一步促使磁场在梯度大的地方集积。这种磁场与温度发展的相互促进关系可以称它为磁扩散不稳定性。本文认为太阳黑子磁环和它低温的形成正是由于这种不稳定性发展起来的。

In this paper, the two-scale analytical method of mean field electrodynamics and some research results, such as α, β effects and α2, α-w solar dynamo models, are reviewed. The main difficulties both in observation and in theory are pinpointed, and the other solar dynamo models are briefly described.

本文介绍了太阳湍流发电机问题的双尺度平均场电动力学分析方法以及有关太阳发电机问题的研究结果:α,β效应及各种发电机模型。总结分析了现阶段太阳湍流发电机问题在观测和理论方面的主要困难。对其他的太阳发电机理论也进行了简要介绍。

 
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