Two-Soliton Solutions of Axially Symmetric Metrics

Stationary axially symmetric solutions of Einstein's field equations generated by the soliton technique are presented in this paper with Laplace's solution as seed. The solutions are asymptotically flat and the Schwarzschild, Kerr and Kerr-NUT metrics are contained in it. The constructed solutions possess an event horizon. The surface area of the event horizon is evaluated. Finally, the solutions presented in this paper are compared with the solutions of Manko. A simple transformation technique is discussed by which one can directly obtain the solutions of Gutsunaev and Manko simply by adjusting a parameter related to the Inverse Scattering Method.     

Axially Symmetric Universe in Creation-Field Cosmology

Axially symmetric space-time is considered in the Hoyle-Narlikar C-field cosmology. Using methods of Narlikar and Padmanabhan (Phys. Rev. D 32:1928, 1985), the solutions have been studied when the creation field C is a function of time t only. The geometrical and physical aspects for models are also studied.     

Constant-Cutoff Approach to Axially Symmetric Dibaryons

We suggest a quantum stabilization method forthe SU(2) -model, based on the constant-cutofflimit of the cutoff quantization method developed byBalakrishna et al., which avoids the difficulties with the usual soliton boundary conditions pointedout by Iwasaki and Ohyama. We investigate the baryonnumber B = 1 sector of the model and show that after thecollective coordinate quantization it admits a stable soliton solution which depends on asingle dimensional arbitrary constant. We then study thedibaryon configurations in this approach, using thegeneralized axially symmetric ansatz to determine the soliton background. Thus we calculate therotational contributions to the masses of the axiallysymmetric dibaryons and show that they are inqualitative agreement with the results obtained usingthe complete Skyrme model. We conclude also that,as in the case of the complete Skyrme model, the lowestallowed S = –2 state has the quantum numbers ofthe H-particle. We find that in the present approach, similarly to the case of the complete Skyrmemodel, this particle is bound, even though the neglectedvacuum effects might contribute to the unbinding of theH-particle.     

Plasma Diagnostics and Nonlinear Wave Studies with a Gridded Electrostatic Energy Analyzer

A simplified theory relating the collector current to the grid bias and other plasma parameters has been developed for a multiple-gridded electrostatic energy analyzer. Experiments have shown that the theory is only approximately valid, but the temperature obtained agrees closely with that from a Langmuir probe. It is found that temperature measurements depend on the grid bias potentials and the ratios of grid hole radius to electron Debye length. As a result, the conditions for the best performance of the energy analyzer as an accurate diagnostic device have been determined. A theory has also been worked out for the second-order change in the electron distribution function due to a cyclotron damped wave. This, together with experimental results, will provide valuable information on the thermal anisotropy of a plasma.     

Axially Symmetric Inflationary Universe in General Relativity

We have investigated a simple axially symmetric inflationary universe in the presence of mass less scalar field with a flat potential. To get an inflationary universe, we have considered a flat region in which potential V is constant. Some physical properties of the universe are also discussed.     

基于MATLAB的静电场模拟

在静电场中引入电位和电场强度后,通过等电位线图和场强分布图可以具体的描述静电场这种抽象的物质场。传统的静电场模拟实验直观地展现出了静电场的分布从而形象地描述了静电场,由于这种方法属于类比模拟,所以存在一定的缺陷(比如不直接,不能描述立体规律等等)。随着计算机技术的发展,利用计算机技术来模拟静电场等物质场逐渐成为趋势。通过借鉴大量资料简要地介绍了如何利用计算机模拟静电场,如何利用MATLAB软件模拟静电场的问题。     

Solar Radiation Scattering by Aerosol Axially Symmetric Objects

We have obtained analytical expressions for the scattering coefficient and the angular distribution of radiation for the aerosol train (tail) modeled by a homogeneous cylinder with given scattering coefficient and phase function of the elementary volume. The analytical formulas for the angular distribution of scattered radiation have been obtained in the single-scattering approximation. Using the Monte Carlo method, we have calculated the directional scattering coefficients of a homogeneous monodisperse tail consisting of spherical water particles with a mean radius of 1 μm for various diametrical optical thicknesses of the tail. The relations obtained can be used for passive remote sensing of aerosol air pollutions. __________ Translated from Zhurnal Prikladnoi Spektroskopii, Vol. 72, No. 5, pp. 604–610, September–October, 2005.     

基于origin软件在静电场数据处理中的应用

传统是采用导电纸来描绘静电场,但描绘的过程中存在不利因素。为提高描绘的精确度,采用不同浓度NaCl溶液,比较不同浓度的导电质液体对静电场描绘的影响。同时利用origin软件对数据处理,探讨溶液浓度对平均精确度的影响。研究表明当NaCl溶液浓度为9%时,平均精确度最大,且origin软件处理数据更简洁和精确。     

Existence of Axially Symmetric Static Solutions of the Einstein-Vlasov System

We prove the existence of static, asymptotically flat non-vacuum spacetimes with axial symmetry where the matter is modeled as a collisionless gas. The axially symmetric solutions of the resulting Einstein-Vlasov system are obtained via the implicit function theorem by perturbing off a suitable spherically symmetric steady state of the Vlasov-Poisson system.     

Energy of Gravitational Field of Static Spherically Symmetric Neutron Stars

By using the Einstein-Tolman expression of the energy-momentum pseudo-tensor, the energy density ofthe gravitational field of the static spherically symmetric neutron stars is calculated in the Cartesian coordinate system.It is exciting that the energy density of gravitational field is positive and rational. The numerical results ot the energydensity of gravitational field of neutron stars are calculated. For neutron stars with M = 2M , the ratio of the energydensity of gravitational field to the energy density of pure matters would be up to 0.54 at the surface.     

Energy of Gravitational Field of Static Spherically Symmetric Neutron Stars

By using the Einstein-Tolman expression of the energy-momentum pseudo-tensor, the energy density of the gravitational field of the static spherically symmetric neutron stars is calculated in the Cartesian coordinate system.It is exciting that the energy density of gravitational field is positive and rational The xmmerical results of the energy density of gravitational field of neutron stars are calculated. For neutron stars with M=2M, the ratio of the energy density of gravitational field to the energy density of pure matters would be up to 0.54 at the surface.     

Cardy-Verlinde Formula for an Axially Symmetric Dilaton-axion Black Hole

It is shown that the Bekenstein-Hawking entropy of an axially symmetric dilaton-axion black hole can be expressed as a Cardy-Verlinde formula. By utilizing first order correction in the Bekenstein-Hawking entropy we find the modified the expressions for the Casimir energy and pure extensive energy. The first order correction to the Cardy-Verlinde formula in the context of dilaton-axion black hole are obtained with the use of modified cosmic and pure extensive energies.     

轴对称变形核中配对粒子态的构成

量子多粒子体系的配对粒子态的构成与体系对称性密切相关.轴对称变形核中的配对粒子态可有三种构成方式,即单极对,±Ω和Signature对,分别是(J2,J3),J3,和(J32,R1(π))的共同本征态.在只计及对力时,三种形式的对力得出的能谱完全相同,常被等价地混用.但在推转壳模型中,由于三种配对态在空间转动下的性质不尽相同,能谱及有关性质随ω的变化将有不同程度的差异.     

Axially Symmetric Bianchi Type-IX Inflationary Universe in General Relativity

Axially symmetric Bianchi type-IX space-time in the presence of mass less scalar field with a flat potential V is investigated. To get an inflationary universe, we have considered a flat region in which potential V is constant. Some physical and kinematical properties of the model are discussed.     

Scalar Field Model of Dark Energy In the Double Complex Symmetric Gravitational Theory

The scalar field model of dark energy is established in the double complex symmetric gravitational theory. The universe we live in is taken as the real part of double complex space M^4C（J）. The two cases of scalar field （ordinary and phantom scalar field） are discussed in a unified way. Not only can the double Friedmann equations be obtained, but also the equation of state for dark energy, potential V（φ） and scalar field φ can be expressed. Hence, a new method is proposed to study dark energy and the evolution of the universe.     

Compact Multichannel Charged-Particle Energy Analyzer Based on a Conical Cut Electrode

Technical Physics - An electrostatic compact analyzer for obtaining the energy spectrum and for detecting simultaneously charged particles in a wide energy range, which is especially important for...     

Vorticity on the Surface of an Axially Symmetric Body behind a Detached Shock Wave

Doklady Physics - The vorticity on the surface of an axially symmetric body streamlined by a steady unswirling homogeneous ideal gas supersonic flow with a detached shock wave has been studied. The...     

An Efficient Dispersion Calculation Method for Axially Symmetric Optical Fibers

An efficient numerical modal calculation method for an axially symmetric optical fiber is presented using a numerical Galerkin's method. By decomposing the transverse electric field of a guided wave with Bessel functions of the first kind in cylindrical polar coordinates, we have shown that dispersion characteristics of an optical fiber can be obtained very easily. In order to illustrate the effectiveness of this suggested method, numerical examples are given for a step index fiber, a W-shape depressed inner cladding fiber, and a dispersion-flattened fiber.     

Rotating,Stationary, Axially Symmetric Spacetimes with Collisionless Matter

The existence of stationary solutions to the Einstein–Vlasov system which are axially symmetric and have non-zero total angular momentum is shown. This provides mathematical models for rotating, general relativistic and asymptotically flat non-vacuum spacetimes. If angular momentum is allowed to be non-zero, the system of equations to solve contains one semilinear elliptic equation which is singular on the axis of rotation. This can be handled very efficiently by recasting the equation as one for an axisymmetric unknown on ${\mathbb{R}^5}$ .