BP L在几条路径上的传播时延和大地等效电导率

本文分析了1984年用搬钟的方法实测 BPL 信号传播时延和场强的结果,得出了在信号地波复盖范围内,根据信号的场强预算传播时延可获得很高的精度,提出了计算时地波传播路径合理分段的基本原则,提出了尚未解决的大城市高大建筑物对信号时延的影响问题。     

山区地形对100KHZ地波相位影响的实验研究

扼要介绍解决不规则地形条件下ＬＦ地波传播问题的积分方程法及其存在问题的诸方面．根据导出方程的基本假设，定性地分析了积分方程应用于地形复杂的山区时会迁到的困难；然后将在秦岭山区实测的地波传播时廷与由积分方程法算得的相应时廷值进行比较，结果表明：在地形沿传播方向（纵向）和垂直于传播方向（横向）的起伏均很急剧的情况下，实测值和计算值偏离很大，相对偏差多数＞５０％，从实验和计算比较说明积分方程法只能用于地波路径的横向地形基本均匀，而纵向地形起伏坡度不超过２０°的不规则地面．文章最后根据实测数据，提出了将山区对地波二次相位因子的影响可以分为路径的山区地形平均影响和接收点附近地形局部影响之和的新概念，并给出了计算局部地形影响的简单方法．用此法得到５个观测点的时延计算值与实测值之差多数＜０．２μｓ．     

100kHz地波计算方法比较

对于无线电授时、导航来说,地球表面大地电特性非常重要,可以用地波衰减法测定大地等效电特性.目前有若干种方法可用于计算100kHz地波场强衰减和二次相位因子随传播路径的距离、大地电特性和大气折射指数的变化.对几种方法计算的结果和采用的参数作了比较和讨论.结果表明:对于1000km距离的均光滑的地球表面的地波传播而言,中国电波研究所的结果与国际电联有关建议书符合得最好.     

罗兰C地波定时精度变化的分析(摘要)

1 定时精度计算方法罗兰C地波定时精度既受发射和接收设备时延的影响,又受到信号传播路径的影响。传播路径时延一般认为只受传播路径上大地导电率和大气折射率的影响。时号时延误差包括系统误差和随机误差,系统误差可通过理论计算和搬运钟比对方法校正;随机误差     

预测地波定时信号传播时延的经验方法

在参考文献（２,３）的基础上,提出了含有大山区的复杂陆地地波路径的分段和确定各段路径等效电导率σｃ的方法,给出如何利用接收点场强实测值和已有的理论色散修正曲线（δｔ－ｄ）＾（６）近似计算色散修正值的方法,并对４条含大山区的复杂路径信号传播时延实测值ｔｇ＾－（收）与预测值ｔｇ进行比较,结果表明：路径分为３段等效时的预测准确度要比整段等效高得多。     

长波传播时延预测中的距离计算问题

本文讨论了目前广泛采用的三种用于地波传播时延计算的大圆距离计算公式,在椭球体面上,这三种公式在一定的近似下被统一起来,并给出了考虑高程时的简单近似公式及忽略高程影响的条件。     

一种基于差分的长波授时方法研究

长波授时具有覆盖范围广、信号传播稳定、抗干扰性能好的特点.长波授时的关键是精确计算长波信号在传播路径上的时间延迟.由于长波传播路径的复杂性以及气象条件的实时性变化,传统的时延预测方法难以实现较高的授时精度.借助于GPS信号,长波定时接收机可以间接获得较精确的传播路径时延.利用长波覆盖范围内相距不远的两接收点具有空间相关性以及传播路径上的电参数近似的特点,计算分析两接收点上传播路径时延的相关系数.在此基础上,提出了一种利用差分进行长波高精度授时的方法,该方法就是利用基准站上预报的差分改正数修正用户点上的传播路径时延.计算结果表明:差分修正后,传播路径时延的预测精度得到一定程度的提高,差分效果明显.这种长波差分授时计算方法可以有效利用传播路径上的公共误差,改善长波时延预测精度,提高长波的授时精度.     

大地坐标的变换与长波传播距离计算

利用长波定时,要求距离计算达到来级精度。本文提供了坐标系统的变换公式,以达到在同一椭球面上进行距离计算。换算到WGS—72椭球面上的坐标值与直接测定的坐标值(在WGS—72椭球面上)相差甚微,两者分别计算到Y台的时延仅有0.017μs的差异。可以满足Loran—C地波传播距离和时延的计算精度。     

无线电长波传播时延的测量

为了在长波授时与导航系统中,进行传播时延的修正,研究电波传播时延修正的理论及方法,及通过传播时延的测量测定土地等效导电率等,必须对电波传播的时延进行精确的测量。利用飞机搬运原子钟方法就是一种高精度的测量长波传播时延的方法。一九七八年十月至十一月进行的3262工程电波传播搬运钟试验,采用飞机搬运铷原子钟测量了我国不同传播路径上许多地点长波天、地波传播的时延,测量的精度为±0.14μs。下面我们就这次实验中传播时延的测量问题进行分析讨论。     

我国大气折射指数梯度对BPL地波时号的影响

本文讨论了我国大气折射指数梯度的分布值及其对BPL地波时号的二次相位因子的影响。采用了我国102个高空气象站十年的实测资料，求得了我国大气折射指数梯度的月平均值，根据这些数值绘制了春秋季、夏季和冬季的《中国大气折射指数梯度分布图》，用这种方法计算的地波时延预测值与地波时延的实测值做了比较，结果表明，本文提供的修正值比标准大气的修正数据更接近实测值。     

关中平原大地等效电导率的间接测量

为准确预报地波传播时延,用电波传播法对关中平原的大地等效电导率进行了间接测量。阐述了电波传播法的测量原理和方法,第一次给出关中平原大地等效电导率的间接测量结果,同时,给出了中国科学院国家授时中心临潼科研楼参考点的BPL信号传播时延测量结果,并对这些测量结果进行了精度分析。     

New mass formula for spherically symmetric stellar configurations

A new formula is derived for the mass of spherically symmetric stellar configurations. An expression will be given where the mass square is connected to an integral over the pressure of gravitating matter. This formula turns out to hold for Newtonian gravity, for Einstein's GRT, for projective and bimetric scalar-tensor and further theories of gravitation.     

Empirical formula to relate the auroral electrojet intensity with interplanetary parameters

An empirical formula has been constructed using the results of correlative analyses to determine in what form the AL index, as a measure of the intensity of the westward auroral electrojet, depends on interplanetary parameters. The formula thus obtained shows that AL is mainly determined by B_sV² where B_s is the southward component of the IMF and V is the solar wind velocity, and is modulated in a characteristic way by the combined effect of the east-west component of the IMF and the tilt angle of the Earth's dipole axis toward the Sun-Earth line. In contrast, effects of the solar wind density and the IMF variability were found to be insignificant.Implications of the empirical formula are discussed mainly in relation to the problem of the location in the dayside magnetosphere of the region where the reconnection process to initiate the substorm takes place.     

一种基于MUSIC算法的天地波识别方法

基于我国BPL长波脉冲信号的特征,利用MUSIC(多信号分类)算法对BPL天、地波延迟进行估计,实现天、地波识别。对传统谱估计IFFT(快速傅里叶逆变换)算法和现代谱估计MUSIC算法进行了仿真和比较,结果表明,这两种方法在较低信噪比条件下可有效分离天、地波,且识别误差都能控制在±5μs内,但MUSIC算法比IFFT算法具有更高的精度和分辨率。     

Inelastic cross section for antihelium on nuclei: an empirical formula for use in the experiments to search for cosmic antimatter

An empirical formula for the cross section for inelastic hadronic interaction of antihelium with nuclei for the projectile energy range from 0.3 GeV/n to 80 GeV/n and target atomic mass number A from 4 to 120 has been developed. It is based on the available experimental data of nucleon (antinucleon) — nucleus and helium — nucleus inelastic cross sections. Such a formula is needed by experiments designed to search for antihelium in cosmic rays. With this formula one can estimate the efficiency of antihelium detection and correct for antihelium attenuation in the atmosphere for the balloon-borne experiments. A byproduct of this work is an empirical formula for antiproton-nucleus inelastic cross.     

Weak discontinuities in relativisitic MHD

By using singular surface theory and ray theory the speeds of propagation of fast and slow waves, propagating into a medium in arbitrary motion, have been obtained in relativistic magnetohydrodynamics. The differential equation governing the growth of these waves along the rays has been derived and the solution has been presented in integral form.     

A new formula describing the scaffold structure of spiral galaxies

We describe a new formula capable of quantitatively characterizing the Hubble sequence of spiral galaxies including grand design and barred spirals. Special shapes such as ring galaxies with inward and outward arms are also described by the analytic continuation of the same formula. The formula is   r (φ) = A /log [ B tan   (φ/2 N )]  . This function intrinsically generates a bar in a continuous, fixed relationship relative to an arm of arbitrary winding sweep. A is simply a scale parameter while B , together with N , determines the spiral pitch. Roughly, greater N results in tighter winding. Greater B results in greater arm sweep and smaller bar/bulge, while smaller B fits larger bar/bulge with a sharper bar/arm junction. Thus B controls the 'bar/bulge-to-arm' size, while N controls the tightness much like the Hubble scheme. The formula can be recast in a form dependent only on a unique point of turnover angle of pitch – essentially a one-parameter fit, aside from a scalefactor. The recast formula is remarkable and unique in that a single parameter can define a spiral shape with either constant or variable pitch capable of tightly fitting Hubble types from grand design spirals to late-type large barred galaxies. We compare the correlation of our pitch parameter to Hubble type with that of the traditional logarithmic spiral for 21 well-shaped galaxies. The pitch parameter of our formula produces a very tight correlation with ideal Hubble type suggesting it is a good discriminator compared to logarithmic pitch, which shows poor correlation here similar to previous works. Representative examples of fitted galaxies are shown.     

Approximate solutions for isothermal flows behind strong spherical shocks with variable energy

Self-similar unsteady flows with zero temperature gradient behind strong spherical shocks propagating in non-uniform perfect gas at rest are investigated. The total energy of the flow is assumed to be varying with the shock radius obeying a power law. Approximate solutions in a closed analytical form are obtained using the integral method. Also these solutions are shown to be useful to calculate easily and quickly the shock temperature, X-ray surface brightness and luminosity which are important in astrophysical problems. It is found that these approximate solutions are in close agreement with numerical solutions.     

Comparative Analysis of VLF Signal Variation along Trajectory Induced by X-ray Solar Flares

Comparative qualitative analysis of amplitude and phase delay variations was carried out along the trajectory of GQD/22.1 kHz and NAA/24.0 kHz VLF signal traces, propagating from Skelton (UK) and Maine (USA) toward Belgrade, induced by four isolated solar X-ray flare events occurred during the period from September 2005 to December 2006. For monitoring, recording and for storage of VLF data at the Institute of Physics in Belgrade, Serbia, the AbsPAL system was used. For modeling purposes of propagating conditions along GQD and NAA signal propagation paths, LWPCv21 program code was used. Occurred solar flare events induced lower ionosphere electron density height profile changes, causing perturbations in VLF wave propagation within Earth-ionosphere waveguides. As analyzed VLF signals characterize by different propagation parameters along trajectories from their transmitters to the Belgrade receiver site, their propagation is affected in different ways for different solar flare events and also for the same solar flare events.     

Linear kinetic theory of instabilities of a gravitatingstellar disk

Linear kinetic theory is developed to describe collective oscillations (and their instabilities) propagating in a rapidly rotating disk of stars, representing a highly flattened galaxy. The analysis is carried out for the special case of a self-gravitating, infinitesimally thin, and spatially inhomogeneous system, taking into account the effects both of thermal movements of stars and of gravitational encounters between stars and giant molecular clouds of an interstellar medium. The star–cloud encounters are described with the use of the Landau collision integral. The dynamics of gravity perturbations with rare interparticle encounters is considered. Such a disk is treated by employing the well elaborated mathematical formalisms from plasma perturbation theory using normal-mode analysis. In particular, the method of solving the Boltzmann equation is applied by integration along paths, neglecting the influence of star–cloud encounters on the distribution of stars in the zeroth-order approximation. We are especially interested in important kinetic effects due to wave–star resonances, which we have little knowledge about. The kinetic effects are introduced via a minor drift motion of stars which is computed from the equations of stellar motion in an unperturbed central force field of a galaxy. The dispersion laws for two main branches of disk's oscillations, that is the classical Jeans branch and an additional gradient branch, are deduced. The resonant Landau-type instabilities of hydrodynamically stable Jeans and gradient gravity perturbations is considered to be a long-term generating mechanism for propagating density waves, thereby leading to spiral-like and/or ring-like patterns in the flat galaxies. This revised version was published online in July 2006 with corrections to the Cover Date.