相经多方球的稳定性

本从理论的角度，讨论了静态相对论多方球的稳定性问题，给出稳定性对球体物质的绝热指数的依赖关系。     

射电喷流中相对论电子束激发的不稳定性

本文作者用相对论电子束在等离子体中运动时的色散关系讨论了纵向传播的波模的稳定性，发现静电Ｌａｎｇｍｕｉｒ波和Ａｌｆｖｅｎ波是不稳定的，并计算了其增长率，而高频电磁模和硝声模是稳定的。相对论电子束激发的Ｌａｎｇｍｕｉｒ波和Ａｌｆｖｅｎ波的不稳定性可用于解释射电喷流中相间的热斑、粒子再加速、辐射机制以及能量传输问题。     

相对论框架里的时间尺度

对国际原子时(TAI),地球力学时(TDT)和质心力学时(TDB)的定义和概念作了回顾和阐述。对其中一些有争议的问题进行了介绍和讨论。我们认为,TAI的建立应当与地心坐标系的选择有关,而把TDT看为是在去除地心引力的虚拟时空中的地心处的原时比较恰当。     

电离层中相对论电子的加速

Stochastic acceleration of an electron in the ionosphere by a standing wave is discussed in the context of the relativistic Hamiltonian formulism. Analysis shows trat the stochasticity is due to the overlap of the two resonances of the electron in the striding wave. The equations of motion arc solved by use of Adams' expector-correcior methods o trace the stochastic motion and stochastic acceleration of the electron.     

相对论岁差章动的理论推导

本文从爱因斯坦场方程的解开始,严格而细致地论证了相对论岁差和章动的起源,推导了测地、Lense-Thirring、Thomas岁差章动和黄极的相对论进动的理论表达式。     

天文地球动力学中的相对论效应

天文地球动力学利用空间与地面观测手段 ,监测和研究地球整体与各圈层的物质运动以及它们间的相互作用 ,这都离不开广义相对论涉及的时间与空间。随着空间对地观测精度的提高 ,为了充分利用高精度观测提供的信息 ,在天文地球动力学的研究中必须考虑相对论效应。所涉及的相对论效应包括 :( 1 )相对论参考系的建立 ,( 2 )在恰当的参考系中对观测者和被观测对象的相对论运动方程 (平动和自转 )的描述 ,( 3 )观测者和被观测对象间的电磁信号传播 ,( 4 )依赖于坐标选择的结果与具有物理意义的可观测量间的转换 ,( 5)某些基本概念与定义在广义相对论框架下的重新确认。本文对天文地球动力学中的这些相对论效应作了简要的评述。     

球单极的引力场和它在谐和坐标条件下的解

本文从球O（3）对称破缺时形成的球单极的外部解，求出了在谐和坐标条件下的解，并在物理上对它们作了简要的讨论。     

On the Stability of Equilibrium Points in the Relativistic Restricted Three-Body Problem

The equilibrium points of the relativistic restricted three-body problem are considered. The stability of the triangular points is determined and contrary to recent results of other authors a region of linear stability in the parameter space is obtained. The positions of the collinear points are approximated by series by expansions and their stability is similarly determined. It is found that these are always unstable.This revised version was published online in October 2005 with corrections to the Cover Date.     

Gravitational Radiation of Relativistic <Emphasis Type="Italic">n</Emphasis> = 1 Polytropes

The gravitational radiation of n = 1 polytropes undergoing quasiradial pulsations is examined. The intensity of the gravitational radiation and the gravitational wave amplitudes are calculated for polytropic models of white dwarfs and neutron stars when the energy of rotation of the object serves as the source of the radiated energy. Calculations of h₀ show that objects with a polytropic equation of state can describe the expected gravitational radiation from white dwarfs and neutron stars. The gravitational radiation of polytropic models of galactic nuclei and quasars is also examined. These objects can create a high enough background of gravitational radiation at frequencies of 10^-8–10^-11 Hz for gravitational wave detectors operating in this frequency range. __________ Translated from Astrofizika, Vol. 48, No. 4, pp. 603–612 (November 2005).     

视超光速运动的相对论超光速模型

从相对论出发，在视超光速源质心相对于观测者静止的条件下，推导出两个向相反方向运动的视超光速子源之间的视速度方程，这一方程包含了相对论射束模型的表现横向速度公式，且对高、低速不同条件均为适用。     

On Relativistic Equations of Motion of an Earth Satellite

For numerical integration of the geocentric equations of motion of Earth satellites in the general relativity framework one may choose now between rather simple equations involving in their relativistic dynamical part only the Earth-induced terms and very complicated equations taking into account the relativistic third-body action. However, it is possible quite easily to take into account the relativistic indirect third-body perturbations and to neglect much lesser direct third-body perturbations. Such approach is based on the use of the Newtonian third-body perturbations in geocentric variables with expressing them in the relativistic manner in terms of the barycentric arguments. Together with it, to extend the known results for the spheroid model of the Earth, the Earth-induced terms are treated in great detail by including the non-spin part of the Earth vector-potential and the Earth triaxial non-sphericity.This revised version was published online in October 2005 with corrections to the Cover Date.     

相对论天体力学和后牛顿运动方程

叙述了与Astrod工程有关的相对论天体力学基础内容。包括相对论天体力学、广义相对论基本原理、PPN方法体系、PPN多体问题、PPN二体问题。高阶PN二体问题等     

Existence and Stability of L4,5 In The Relativistic Restricted Three-Body Problem

The existence and stability of triangular libration points in the relativistic restricted three-body problem has been studied. It is found that L_4,5 are unstable in the whole range 0 ≤ μ ≤ 1/2 in contrast to the classical restricted three-body problem where they are stable for 0 < μ < μ₀, where μ is the mass parameter and μ₀ = 0.03852.... This revised version was published online in July 2006 with corrections to the Cover Date.     

Relativistic magnetofluid disc with nonzero radial velocity in Schwarzschild geometry

In this paper we consider the equilibrium of a magnetofluid disc in Schwarzschild background with an external magnetic field, having the azimuthal and the radial components of the flow velocity nonzero. The electrical conductivityσ of the fluid is taken to be finite and thus the solution for the electromagnetic field is required to satisfy the Ohm’s law too with the four-current having onlyJ ^ϕ andJ ^t nonzero. The various physical parameters that have to correlate for possible equilibrium configurations are identified and their respective magnitudes estimated. It is found that for a given angular momentum distribution the inner edge of the disc can reach well within the usual6m limit only when the surface magnetic field of the central object is not too high when the matter density at the outer edge of the disc and the accretion rate are taken with reasonable limits     

Relativistic beaming in the central components of double radio quasars

Using a large sample of 78 well-observed double quasars, we have investigated several consequences of the relativistic beaming model. In this model the ratio of the strengths of the central component and outer lobes of a double source depends on whether the jet axis lies close to or away from the line of sight, If this is the actual situation, the fraction of emission from the core,f _c, may be used as a statistical measure of the orientation of the source and should be correlated with other source parameters which also depend on the inclination of the jet axis to the line of sight. We findf _c to be anticorrelated with the overall projected linear size of the extended emission but to exhibit a positive correlation with both the observed degree of misalignment from a collinear double structure, and the ratio of separations of the outer hotspots from the central component. As might be expected from these relationships, we also find sources of smaller projected linear sizes to appear more misaligned and the degree of misalignment to be correlated with the ratio of separations of the outer hotspots. All these correlations are consistent with the predictions of the relativistic beaming model.     

Electromagnetic Field of a Cylinder with a Periodic Current: Energy Flux from a Relativistic Jet

An exact solution is obtained for the electromagnetic field surrounding an infinitely long, conducting cylinder with a periodic axial electric current. The solution simultaneously gives the field near the cylinder and in the transition to the wave zone. The flux of electromagnetic radiation emitted by the cylinder is calculated for oscillations with long wavelengths greatly exceeding the radius of the cylinder. This solution can be used to describe the electromagnetic field around narrowly collimated jets from active galactic nuclei and quasars.     

Dispersion Relation of Longitudinal Oscillations in Relativistic Plasmas of Fast Electron Distribution

In the relativistic case, the dispersion equation of longitudinal oscillations in unmagnetized, collisionless and isotropic plasmas of fast electron distribution is derived from the longitudinal dielectric constant of plasma. The equation is analytically solved, and the long-wavelength and short-wavelength dispersion relations are obtained. Because of the discontinuity of the analytical dispersion curve, the dimensionless dispersion equation of longitudinal oscillations is numerically calculated to obtain the full dispersion curve of longitudinal oscillations in relativistic plasmas of fast electron distribution. Further more, by fitting the numerical solution, a simple functional expression of the dispersion curve is given in favor of applications. Finally, in the extremely relativistic case, the dispersion relation of fast electron distribution is compared with that of Maxwell distribution. It is shown that the two kinds of dispersion relations have similar properties in a certain range of wave numbers.