Von Karman 型自相关函数模拟随机介质

利用Von Karman型自相关函数建立了随机介质模型,对自相关长度、谱指数两个参量分别讨论了模型的特征,分析了不同扰动标准差下模型 中速度的分布和变化情况。结果显示：改变自相关长度及横纵向谱指数,都可以产生横向和纵向上非均匀体尺度改变的随机介质模型;扰动标准差 不同,得到的随机扰动的范围就不同,从而引起模型中速度围绕背景速度上下波动。从模拟结果图显示,随机介质模型能灵活地描述实际介质。     

Spectral Simulation of Isotropic Gaussian Random Fields on a Sphere

A spectral algorithm is proposed to simulate an isotropic Gaussian random field on a sphere equipped with a geodesic metric. This algorithm supposes that the angular power spectrum of the covariance function is explicitly known. Direct analytic calculations are performed for exponential and linear covariance functions. In addition, three families of covariance functions are presented where the calculation of the angular power spectrum is simplified (shot-noise random fields, Yadrenko covariance functions and solutions of certain stochastic partial differential equations). Numerous illustrative examples are given.

     

Inverse solution to the wave equation using the Laguerre transform

An inverse solution to the 1D wave equation is obtained using the spectral Laguerre transform to find the distribution of wave velocities at some point of the medium. The problem is solved as optimization in which the function of Laguerre harmonics is minimized by the conjugate gradient or Newton’s algorithms.Reported are velocities of a wave defined by a stepwise constant function. The accuracy of the inverse solution for the Laguerre harmonics is investigated against the approximation accuracy in the boundary problem. The accuracy and efficiency of the Laguerre method are compared to those in the Fourier method.     

The cyclotron spectrum of anisotropic ultrarelativistic electrons: Interpretation of X-ray pulsar spectra

The spectrum of cyclotron radiation produced by electrons with a strongly anisotropic velocity distribution is calculated taking into account higher harmonics. The motion of the electrons is assumed to be ultrarelativistic along the magnetic field and nonrelativistic across the field. One characteristic feature of the resulting spectrum is that harmonics of various orders are not equally spaced. The physical properties and observed spectra of four X-ray pulsars displaying higher cyclotron harmonics are analyzed. It was shown that at least in one of them, the cyclotron feature can apparently be only an emission line. Moreover, the observed harmonics are not equidistant, and display certain other properties characteristic of emission by strongly anisotropic ultrarelativistic electrons. In addition, there are indirect theoretical arguments that the electrons giving rise to cyclotron features in the spectra of X-ray pulsars are ultrarelativistic and characterized by strongly anisotropic distributions. As a result, estimates of the magnetic fields of X-ray pulsars (which are usually derived from the energies of cyclotron lines) and certain other physical parameters require substantial revision.     

Studies of the Angular Structure of Scintillating Radio Sources at 111 MHz

The angular sizes and compactnesses of 53 scintillating radio sources observed at 111 MHz on the Large Phased Array of the Lebedev Physical Institute are estimated. The parameters of the angular structures of the sources are estimated using a new method based on a joint analysis of the scintillation index and the asymmetry coefficient for the statistical distribution of the intensity fluctuations. The asymmetry coefficient for scintillations of a point source is estimated based on an analysis of observational data for turbulence in the solar wind. Different methods for estimating source angular sizes based on observations of interplanetary scintillations are compared. It is shown that the proposed new method is suitable for sources with angular sizes up to 1″. The accuracy of the estimated angular sizes and compactnesses of the sources is about 40%.

     

The possible escape of electron cyclotron maser radiation from hot stellar coronas through a window of transparency

The main argument against the idea that the intense radio emission observed from active regions on the Sun and flare stars is electron-cyclotron maser (ECM) radiation is that such radiation should be strongly absorbed in higher-lying layers where the condition for the cyclotron resonance at harmonics of the electron gyrofrequency is fulfilled. Cyclotron absorption lowers the efficiency of ECM radiation virtually to zero for a broad range of angles between the direction of propagation of the radiation and the magnetic field. Less severe absorption is possible only in narrow angular “windows” along (for ordinary and extraordinary waves) and perpendicular to (for ordinary waves) the magnetic field. However, the ECM radiation that is generated does not fall into these windows of transparency due to the kinematic conditions corresponding to coronal magnetic traps. We investigate the efficiency of induced scattering of ECM radiation on ions in the equilibrium plasma in the source. Under certain conditions, induced scattering leads to the formation of a condensate of ECM radiation with the direction of its wave vectors approximately along the magnetic field, enabling the escape of the radiation through windows of transparency. The most favorable conditions for this phenomenon are realized for ordinary waves. We estimate the optical depths of the sources of the ECM radiation to the scattering and the angular width of the condensate for ordinary and extraordinary waves for the cases of the flare radio emission of the star AD Leo and the sources of type I noise storms in the solar corona. In both cases, the polarization of the emergent radiation should correspond to the ordinary wave.     

A high-accuracy method for the removal of point sources from maps of the cosmic microwave background

A new method for removing point radio sources and other non-Gaussian noise is proposed as a means of improving the accuracy of estimates of the angular power spectrum of the cosmic microwave background (CMB). The main idea of the method is to reconstruct fluctuations of the CMB in places contaminated by such emission, while traditional methods simply exclude these regions from consideration, leading to the appearance of “holes” in the resulting maps. The fundamental possibility of reconstructing the CMB signal in such holes follows from the analytical properties of a function with a finite spatial spectrum (the Silk damping frequency). A two-dimensional median filter is used to localize the point radio sources. Results of simulations of the method for maps of modest size are presented. The efficiency of applying the method to reconstruct the CMB from data with limited resolution and contaminated by appreciable pixel noise is investigated. The fundamental possibility of applying the method to reconstruct the CMB distribution in the region of the Galaxy is also demonstrated.     

The OSACA database and a kinematic analysis of stars in the solar neighborhood

We transformed radial velocities compiled from more than 1400 published sources, including the Geneva-Copenhagen survey of the solar neighborhood (CORAVEL-CfA), into a uniform system based on the radial velocities of 854 standard stars in our list. This enabled us to calculate the average weighted radial velocities for more than 25000 HIPPARCOS stars located in the local Galactic spiral arm (Orion arm) with a median error of ±1 km/s. We use these radial velocities together with the stars’ coordinates, parallaxes, and proper motions to determine their Galactic coordinates and space velocities. These quantities, along with other parameters of the stars, are available from the continuously updated Orion Spiral Arm Catalogue (OSACA) and the associated database. We perform a kinematic analysis of the stars by applying an Ogorodnikov-Milne model to the OSACA data. The kinematics of the nearest single and multiple main-sequence stars differ substantially. We used distant (-r ≈ 0.2 kpc) stars of mixed spectral composition to estimate the angular velocity of the Galactic rotation, ω_o = ?25.7 ± 1.2 kms^?1 kpc^?1, and the vertex deviation, l = 13° ± 2°, and detected a negative K effect. This negative K effect is most conspicuous in the motion of A0–A5 giants and is equal to K = ?13.1 ± 2.0 kms^?1 kpc^?1.     

Apparent angular sizes of the sources of microwave subsecond pulses and electron-density fluctuations in the lower solar corona

Data on the visible angular sizes of sources of microwave subsecond pulses (MSPs) obtained using the Siberian Solar Radio Telescope are analyzed assuming a dominant role for scattering on small-scale electron-density inhomogeneities in the solar corona. The observed dependence of the angular sizes of MSPs on the distance from the solar-disk center confirms that the MSP sources are localized in low layers of the solar corona. Both absolute and fractional levels of small-scale electron-density fluctuations have been estimated. These estimates suggest that flicker-noise-type turbulence power spectra are formed in the lower corona, and are preserved in the solar-wind acceleration region. A composite dependence of the scattering angle of a sounding radio wave on distance from the Sun is presented.     

Dynamics of gaseous disks in a non-axisymmetric dark halo

The dynamics of a galactic disk in a non-axisymmetric (triaxial) dark halo is studied in detail using high-resolution, numerical, hydrodynamical models. A long-lived, two-armed spiral pattern is generated for a wide range of parameters. The spiral structure is global, and the number of turns can be two or three, depending on the model parameters. The morphology and kinematics of the spiral pattern are studied as functions of the halo and disk parameters. The spiral structure rotates slowly, and its angular velocity varies quasi-periodically. Models with differing relative halo masses, halo semi-axis ratios, distributions of matter in the disk, Mach numbers in the gaseous component, and angular rotational velocities of their halos are considered.     

Study of Bright Compact Radio Sources of the Northern Hemisphere at 111 MHz

The search for compact components of strong ($${{S}_{{{\text{int}}}}} \geqslant 5$$ Jy at 102.5 MHz) discrete radio sources from the Pushchino catalogue was carried out using the method of interplanetary scintillation. A total of 3620 sources were examined, and 812 of them were found to harbor compact (scintillating) components. Estimates of fluctuations of the flux density of these compact components were derived from the scintillation index ($${{m}_{{\max}}}$$) corresponding to an elongation of 25°. The angular size and compactness of 178 sources with compact components were estimated. Scintillation indices of sources corresponding to the compact component ($${{m}_{0}}$$) and flux densities of compact components were determined. It was demonstrated that slow variations of the spatial distribution of interplanetary plasma, which are related to the 11-year cycle of solar activity, may exert a systematic influence on the estimates of angular sizes of sources. Coefficients compensating the deviation from the spherical symmetry of solar wind in the estimates of angular sizes were found using the coefficient of asymmetry of the statistical distribution of intensity fluctuations. The study of correlations between the parameters of sources in the sample revealed that the maximum value of the scintillation index decreases as the integrated flux increases, while the angular size has no marked dependence on the integrated flux.     

利用爆炸震源资料获得三分量旋转地震动

三分量旋转地震动是目前地球物理研究重点之一.利用爆炸震源的平动地震仪观测资料,通过间接计算获得三分量旋转地震动.利用了3炮500 kg炸药的观测资料,3个爆炸点到观测台阵的距离分别是1.8、2.8和8.9 km,计算得到了台阵相对于这3个爆炸点的旋转地震动,其最大峰值旋转角速度分别是41.65、21.98和0.29 μrads/s,与国际同行的旋转地震动结果量级接近.地震动峰值随震中距的衰减是地震工程中关注的问题.提取出三分量的旋转角速度峰值,利用指数函数对三分量的峰值进行拟合,初步得到三分量的旋转地震动角速度峰值随震中距的衰减关系.衰减曲线的主要特征是,1~3 km旋转角速度能量迅速衰减,大于5 km以后衰减逐渐减慢,随着震中距增大曲线的变化越来越趋于平缓.      

Compact radio sources and interstellar scattering near the galactic center

Using literature data on approximately 400 compact radio sources detected with the Very Large Array and located in the direction of the Galactic center within 2° of the compact source Sgr A*, 69 sources whose angular sizes are determined by scattering on electron density inhomogeneities were distinguished. Fifty-five of these are extragalactic, two are supercompact HII regions, ten are sources of maser emission, and two are variable Galactic sources. The excess of the apparent angular sizes of maser sources within 2° of the Galactic center above the mean size of objects of this class in other parts of the Galaxy found in many studies cannot be explained purely by the effect of scattering of their radio emission on interstellar plasma inhomogeneities. The angular sizes of these objects are increased due to scattering only within Galactic longitudes of about 0.4° and Galactic latitudes less than 0.1°. The turbulent medium responsible for scattering of radio emission of compact sources in the immediate vicinity of the Galactic center is strongly concentrated toward the compact source Sgr A* at the Galactic center. No extragalactic sources are observed within 0.4° in longitude and 0.2° in latitude of the Galactic center, because of their low brightness due to the superstrong scattering in this region. Data on scatter broadening can be used to study the distribution of turbulent plasma near the Galactic center.     

Measurement and Analysis of Ground Vibration with Various Sources at Iron and Steel Complex

In this paper, the measurement technique and analysis method of ground vibration with various sources at iron and steel complex are described. The practical measurement cases of ground vibration excited by gas compressor, hammer, truck, train etc. at iron and steel complex are presented. The shapes of wave velocity, peak values, and the main frequency from measured point are listed. The measurement results point out that the velocity waves with different sources have different forms, which are mainly divided the wave forms into three types : the complex-steady-state wave, the shock wave, and the random wave, different main frequency spectrum, different peak values of velocity, and different decay law with distance from sources. The wave in three directions have different forms at each measured point with same seismic source, and their decay laws are different, too. The decay laws of vertical displacements caused by fallen-hammer with the distance from source quite fit in with the equation derivative by Bornitz.     

钢铁联合企业各种振源地基振动的测量与分析

本文叙述了钢铁联合企业内各种振源地基振动的测量技术和分析方法,介绍了武钢等企业内空气压缩机、落锤、锻锤、汽车、火车等振源地基振动的实测情况,列出了各测点的速度波形、峰值、主频等数据。实测表明:不同的振源具有不同的振动波形(大致分为复合稳态波、冲击波、随机波三类)、不同的主频率带、不同的速度峰值及其随距离衰减的规律,且同一振源各测点上三个方向的振动波形不同,衰减规律也不同。落锤振源各测点垂直位移随距离的衰减规律与博尼茨(Bornitz)推导的关系式比较符合。     

Gas kinematics in high-mass star-forming regions from the Perseus spiral arm

We present results of a survey of 14 star-forming regions from the Perseus spiral armin CS (2–1) and ¹³CO (1–0) lines with the Onsala Space Observatory 20 m telescope. Maps of 10 sources in both lines are obtained. For the remaining sources a map in just one line or a single-point spectrum is obtained. On the basis of newly obtained and published observational data we consider the relation between velocities of the “quasi-thermal” CS (2–1) line and 6.7 GHz methanol maser line in 24 high-mass star-forming regions in the Perseus arm. We show that, surprisingly, velocity ranges of 6.7 GHz methanol maser emission are predominantly red-shifted with respect to corresponding CS (2–1) line velocity ranges in the Perseus arm. We suggest that the predominance of the “red-shifted masers” in the Perseus arm could be related to the alignment of gas flows caused by the large-scalemotions in the Galaxy. Large-scale galactic shock related to the spiral structure is supposed to affect the local kinematics of the star-forming regions. Part of the Perseus arm, between galactic longitudes from 85° to 124° , does not contain blue-shifted masers at all. Radial velocities of the sources are the greatest in this particular part of the arm, so the velocity difference is clearly pronounced. ¹³CO (1–0) and CS (2–1) velocity maps of G183.35-0.58 show gas velocity difference between the center and the periphery of the molecular clump up to 1.2 km s^?1. Similar situation is likely to occur in G85.40-0.00. This can correspond to the case when the large-scale shock wave entrains the outer parts of a molecular clump in motion while the dense central clump is less affected by the shock.     

Parameters of the turbulence of the interplanetary plasma derived from scintillation observations of the quasar 3C 48 at the solar-activity minimum

Temporal spectra of interplanetary scintillations of the strong radio source 3C 48 based on 111 MHz observations on the Large Scanning Antenna of the Lebedev Physical Institute obtained near the solar-activity minimum are analyzed. Measurements of the temporal spectrum of the scintillations are used to estimate the angular size of the source, the velocity of inhomogeneities, and the power-law index for the spatial spectrum of the turbulence in the interplanetary plasma. The mean angular size of the source is θ ₀ = 0.326″ ± 0.016″, and the mean index for the three-dimensional turbulence spectrum is n = 3.7 ± 0.2. There is some evidence that n decreases in the transition from the fast, high-speed to the slow, low-latitude solar wind.     

The magnetic fields and angular sizes of radio sources displaying synchrotron self-absorption

A method for estimating the magnetic-field strengths and angular sizes of radio sources displaying synchrotron self-absorption based on their observed radio spectra is considered. The method is used to derive the angular sizes of compact radio sources (components) and the magnetic fields in these regions, as well as the energy and number of relativistic electrons and the radiative power of a number of quasars and radio galaxies.     

Tidal and Nontidal Oscillations in Elkhorn Slough,CA

Elkhorn Slough is a shallow, tidally forced estuary that is directly connected to Monterey Bay. It is ebb-dominated and, due to continued erosion, the tidal prism has tripled over the past 40 years. Water level measurements at four locations are used to examine tidal and nontidal oscillations in Elkhorn Slough. The tidal response of Elkhorn Slough differs from that of Monterey Bay primarily due to the generation of a relatively large number of shallow-water tidal constituents that are due to tidal distortion caused by friction along the bottom and lateral boundaries, intertidal storage, and nonlinear advection. The shallow-water constituents range from 3 to almost 15 cycles per day (cpd) and include a rich variety of overtides and compound tides, whose amplitudes generally increase toward the head of the slough. The tidal harmonics are seasonally dependent, with lower amplitudes during the fall and winter and higher amplitudes in summer. The tidal constituents were examined using two types of spectral decomposition, the conventional power spectrum and the more recent Hilbert spectrum. Unlike the power spectrum, the Hilbert spectrum does not reveal any harmonic structure in the data. Energy associated with tidal distortion in this case appears to be broadly distributed across the spectral continuum. At least four nontidal oscillations occur in Elkhorn Slough with frequencies of 26.0, 39.7, 52.7, and 66.9 cpd. The Hilbert spectrum reveals maxima at 26, 39.7, and 66.9 cpd, but not at 52.7 cpd, suggesting that it is harmonically related to the oscillation at 26.0 cpd. The nontidal oscillations fall into the range of frequencies associated with the natural oscillations of Monterey Bay. However, evolutionary power spectra indicate that they appear to be permanent features of the system and thus are not necessarily consistent with seiche-like oscillations that are often transient and subject to damping. These oscillations could be caused by several factors including edge waves along the coast of Monterey Bay, long-period surface waves of atmospheric origin that enter the bay from offshore, or breaking internal waves in and around the Monterey Submarine Canyon. In conclusion, detailed hydrodynamic models are needed to provide a better understanding of how tidal harmonics are generated and preserved in Elkhorn Slough, and to determine the origin of the natural oscillations in Monterey Bay.     

GAMMA-400 Project

Extraterrestrial gamma-ray astronomy is now a source of a new knowledge in the fields of astrophysics, cosmic-ray physics, and the nature of dark matter. The next absolutely necessary step in the development of extraterrestrial high-energy gamma-ray astronomy is the improvement of the physical and technical characteristics of gamma-ray telescopes, especially their angular and energy resolutions. Such a new generation telescope will be GAMMA-400, currently under development. Together with an X-ray telescope, it will perform precise and detailed observations in the energy range of ~20 MeV to ~10 000 GeV and 3–30 keV the Galactic plane, especially, toward the Galactic Center, Fermi Bubbles, Crab, Cygnus, etc. The GAMMA-400 will operate in the highly elliptic orbit continuously for a long time with the unprecedented angular (~0.01? at E_γ = 100 GeV) and energy (~1% at E_γ = 100 GeV) resolutions, exceeding the Fermi-LAT as well as ground-based gamma-ray telescopes by a factor of 5–10. GAMMA-400 will permit resolving gamma rays from annihilation or decay of dark matter particles, identifyingmany discrete sources (many of which are variable), clarifying the structure of extended sources, specifying the data on the diffuse emission, as well as measuring electron + positron fluxes and specifying electron + positron spectrum in the energy range from 1 GeV to 10 000 GeV.