Simulations of the anisotropic kinetic and magnetic alpha effects     

A. Brandenburg  K. Subramanian 《Astronomische Nachrichten》2007,328(6):507-512

Using simulations of isotropically forced helical turbulence the contributions to kinetic and magnetic alpha effects are computed. It is shown that for the parameter regimes considered in an earlier publication (Brandenburg & Subramanian 2005), the expressions for isotropic and anisotropic alpha effects give quantitatively similar results. Both kinetic and magnetic alpha effects are proportional to a relaxation time whose value, in units of the turnover time, is shown to be approximately unity and independent of the magnetic Reynolds number. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Dispersive shock waves in the solar wind     

I. Ballai  E. Forgcs‐Dajka  A. Marcu 《Astronomische Nachrichten》2007,328(8):734-737

Compressional waves in the solar wind propagating over large distances are likely to steepen into shock waves where the increase in the amplitude is balanced by dissipation. Dispersive effects caused by, e.g. Hall currents perpendicular to the ambient magnetic field can influence the generation and propagation of shock waves. In the present study the dispersion is considered weak but in time its importance can grow. When the effect of dispersion is strong enough, it can balance the nonlinear steepening of waves leading to the formation of solitons. The obtained results show that the weak dispersion will alter the amplitude and propagation speed of the shock wave. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Dynamo action in simulations of penetrative solar convection with an imposed tachocline     

M.K. Browning  A.S. Brun  M.S. Miesch  J. Toomre 《Astronomische Nachrichten》2007,328(10):1100-1103

We summarize new and continuing three-dimensional spherical shell simulations of dynamo action by convection allowed to penetrate downward into a tachocline of rotational shear. The inclusion of an imposed tachocline allows us to examine several processes believed to be essential in the operation of the global solar dynamo, including differential rotation, magnetic pumping, and the stretching and organization of fields within the tachocline. In the stably stratified core, our simulations reveal that strong axisymmetric magnetic fields (of ∼ 3000 G strength) can be built, and that those fields generally exhibit a striking antisymmetric parity, with fields in the northern hemisphere largely of opposite polarity to those in the southern hemisphere. In the convection zone above, fluctuating fields dominate over weaker mean fields. New calculations indicate that the tendency toward toroidal fields of antisymmetric parity is relatively insensitive to initial magnetic field configurations; they also reveal that on decade-long timescales, the magnetic fields can briefly enter (and subsequently emerge from) states of symmetric parity.We have not yet observed any overall reversals of the field polarity, nor systematic latitudinal propagation. (© 2007 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

线状对流中EF3级强龙卷的多尺度机理研究     

张楠  杨晓君  林晓萌  李彩玲  王莹 《气象》2020,46(7):873-884

利用NCEP再分析资料、地面观测资料、多普勒雷达资料、风廓线雷达资料、FY-4A卫星资料、雷达变分同化分析系统输出的高分辨率分析场资料对2018年8月13日17:30发生在天津静海地区的EF3级强龙卷过程进行分析,结果表明:此次过程为发生在线状对流中的强龙卷,且引发龙卷的对流风暴不具备超级单体风暴典型特征,龙卷形成后,在涡旋不断加强的基础上,旋转中心不断下降,且TVS的伸展厚度不断增大。两个线状对流之间新单体的形成发展促使了线状对流的合并,新生对流单体强回波接地时间与龙卷的发生时间有较好的对应关系。在龙卷发生前20 min,分别位于两条边界层辐合线北侧和西侧的偏北风和前方入流的偏东风构成了中低压的辐合旋转流场,当雷暴出流与龙卷发生地的局地风垂直切变中心(在180 m高度可达90×10~(-3)s~(-1))相遇,辐合线上水平分布极不均匀的上升运动迫使水平涡管倾斜,加强了垂直涡度,涡管在垂直方向上被拉伸,根据角动量守恒,旋转加强形成龙卷母体涡旋,因此,发生在线状对流中的强龙卷虽然在对流模态上与超级单体龙卷不同,但龙卷母体涡旋形成的物理机理是一致的。  相似文献   

木星“大红斑”的旋转浅水实验模拟研究   总被引：1，自引：0，他引：1  

王振坡  王丽艳  刘书声 《天文学报》2001,42(4):397-407

在具有自由表面的旋转轨物面浅水实验系统上进行了可重复的系列模拟实验，在旋转随动坐标系中拍摄的照片和功率谱分析表明，确有大尺度持续存在的涡旋、漂移与演化产生，在一定条件下，呈现出一个自持的、长寿命的、沿与整体旋转方向相反方向漂移的反气旋孤立波涡旋（Rossby孤立波涡旋），这就是木星“大红斑”的实验室模型，实验结果证实，流体动力学不稳定主要来自于剪切和Coriolis力效应，由于远离平衡态的耗散系统的自组织，涌现出大尺度长寿命相干涡旋结构，受多次实验的启发，从流体动力学基本方程出发，在一定的实验条件下提出一个半经验模型，近似求出了Rossby孤立波涡旋解。  相似文献   

Lines formed in rotating and expanding atmospheres     

A. Peraiah 《Journal of Astrophysics and Astronomy》1980,1(1):17-23

Spectral lines formed in a rotating and expanding atmosphere have been computed in the frame of the observer at infinity. Two kinds of velocity laws are employed: (i) a uniform radial velocity of the gas and (ii) velocity increasing with radius (i.e. velocity gradients). The atmosphere has been assumed to be rotating with constant velocity. We have considered maximum radial and rotational velocities to be 10 and 3 mean thermal units respectively in an atmosphere whose geometrical thickness is 10 times the stellar radius. The total radial optical depth at line centre is taken to be about 100. In all cases, Doppler profile and a source function which is varying as 1/r ² have been used. Generally, the lines are broadened when rotation is introduced. However, when radial motion is also present, broadening becomes asymmetric and the red emission and blue absorption are enhanced.  相似文献   

Chemical spots and oscillatory diffusion modes in magnetic stars     

V. Urpin 《Astronomische Nachrichten》2016,337(6):633-639

The stars of the middle main sequence often have spot‐like chemical structures at their surfaces. We consider diffusion caused by electric currents and argue that such current‐driven diffusion can form chemical inhomogeneities in a plasma. The considered mechanism can contribute to a formation of element spots in Hg‐Mn and Ap‐stars. Due to the Hall effect, diffusion in the presence of electric currents can be accompanied by the propagation of a particular type of magnetohydrodynamic modes in which only the impurity number density oscillates. Such modes exist if the magnetic pressure is much greater than the gas pressure and can be the reason for variations of the abundance peculiarities in stars. (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

The Tayler instability of toroidal magnetic fields in a columnar gallium experiment     

G. Rüdiger  M. Schultz  M. Gellert 《Astronomische Nachrichten》2011,332(1):17-23

The nonaxisymmetric Tayler instability of toroidal magnetic fields due to axial electric currents is studied for conducting incompressible fluids between two coaxial cylinders without endplates. The inner cylinder is considered as so thin that the limit of R_in → 0 can be computed. The magnetic Prandtl number is varied over many orders of magnitudes but the azimuthal mode number of the perturbations is fixed to m = 1. In the linear approximation the critical magnetic field amplitudes and the growth rates of the instability are determined for both resting and rotating cylinders. Without rotation the critical Hartmann numbers do not depend on the magnetic Prandtl number but this is not true for the corresponding growth rates. For given product of viscosity and magnetic diffusivity the growth rates for small and large magnetic Prandtl number are much smaller than those for Pm = 1. For gallium under the influence of a magnetic field at the outer cylinder of 1 kG the resulting growth time is 5 s. The minimum electric current through a container of 10 cm diameter to excite the instability is 3.20 kA. For a rotating container both the critical magnetic field and the related growth times are larger than for the resting column (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Modeling spatio‐temporal nonlocality in mean‐field dynamos     

M. Rheinhardt  A. Brandenburg 《Astronomische Nachrichten》2012,333(1):71-77

When scale separation in space or time is poor, the mean‐field α effect and turbulent diffusivity have to be replaced by integral kernels by which the dependence of the mean electromotive force on the mean magnetic field becomes nonlocal. Earlier work in computing these kernels using the test‐field method is now generalized to the case in which both spatial and temporal scale separations are poor. The approximate form of the kernel for isotropic stationary turbulence is such that it can be treated in a straightforward manner by solving a partial differential equation for the mean electromotive force. The resulting mean‐field equations are solved for oscillatory α –shear dynamos as well as α² dynamos with α linearly depending on position, which makes this dynamo oscillatory, too. In both cases, the critical values of the dynamo number is lowered due to spatio‐temporal nonlocality.When scale separation in space or time is poor, the mean‐field α effect and turbulent diffusivity have to be replaced by integral kernels by which the dependence of the mean electromotive force on the mean magnetic field becomes nonlocal. Earlier work in computing these kernels using the test‐field method is now generalized to the case in which both spatial and temporal scale separations are poor. The approximate form of the kernel for isotropic stationary turbulence is such that it can be treated in a straightforward manner by solving a partial differential equation for the mean electromotive force. The resulting mean‐field equations are solved for oscillatory α –shear dynamos as well as α² dynamos  相似文献   

Buoyant boundary layer flows- an analogy to the Ekman spiral     

Jae Min Hyun 《地球物理与天体物理流体动力学》2013,107(2):89-98

Abstract

Flow details inside the buoyant boundary layer in the heat-up process of a contained, stably stratified, fluid are presented. Numerical solutions were obtained for the heatup problem in a cylinder considered by Sakurai and Matsuda (1972). By plotting the scaled vertical velocity W versus the scaled temperature θ as functions of the normal distance from the sidewall, the precise shape of the buoyant layer spiral is constructed. The analogy between this spiral and the Ekman spiral in rotating fluids is apparent. As the Rayleigh number Ra increases, the magnitude of the scaled vertical velocity increases substantially, but the scaled temperature does not vary appreciably. The buoyant layer thickness is determined by measuring the zero-crossing normal distance for the vertical velocity. The buoyant layer suction increases significantly as Ra increases. The effects of vertical level and of time on the qualitative behavior of buoyant layer flows are found to be small. The buoyant layer flows decay over the heat-up time scale t _n ; t _h characterizes the time span over which the overall adjustment process in the inviscid interior region is accomplished. This work clarifies that the analogy between heat-up and spin-up, which has been known to exist in the main body of inviscid fluid, applies equally well to the boundary layer regions.  相似文献