О лагранжевых и зйлеровых решеиях обощенной задачи трех тел

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This paper is a continuation and a generalization of one published earlier (Duboshin, 1969): it discusses the problem whether there exist the Lagrangian and the Eulerian solutions of the generalized three-body (material points) problem. Every point in this generalized problem acts on another, one with a force (attractive or repulsive) directed along the straight line passing through these points, and in an arbitrary manner depending on time, mutual distance and its derivatives, the first and the second. Here, generally speaking, the third axiom of dynamics (law of action and reaction) is not presupposed as fulfilled, that is, it is supposed that every two material points interact in a different way.This most general assumption being made, we establish the conditions which must dictate the laws of the interactions, so that the three points can always remain at the apexes of the equilateral triangle (Langrangian solution), or remain always on a straight line (Eulerian solution).The author believes that such general treatment of the three-body problem can be useful for theoretical studies in celestial mechanics and also for practical applications in the study of isolated stellar systems.

     

Hubble expansion in a euclidean framework

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Динамические равновесные плазменные конфигуации и физика магнитосферы

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Несколько замечаний о гамма-излучении и химическом составе квазаров

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МасштаБ и напряженность галактического магнитного поля поданньым пулБсаров

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Магнитное поле вращающегося оБлака и магнито-ротационные взрывы

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О природе всплесков γ-излучения

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On a possible mechanism responsible for the differential energy spectrum of relativistic electrons and non-linear low-frequency spectra of cosmic radio sources

The paper suggests an explanation of the deviations from the power law which are observed in frequency spectra of discrete radio sources at decametric wavelengths. It has been shown that a possible mechanism of the deviations is a combined effect of the stimulated and spontaneous scattering of relativistic electrons in the turbulent plasma of a source, as well as ionization energy losses thereof. The distribution function of the relativistic electrons, empirically established in an earlier paper (Braudeet al., 1971) has been derived from the kinetic equation. For a number of discrete sources the turbulence energy density and the plasma concentration are deduced with the aid of experimental data on low-frequency radio spectra.

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Сешение плоской задачиn неподвишньих центров

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For a special choice of parameters the plane problem of the motion of a passively gravitating material point in the gravitation field ofn fixed centres is reduced to quadratures.

     

Оптимальное демпфирование нутационного движения спутников, стаБилизируемых вращением

, . , , . , , -, This article investigates the dynamics of a system for damping the nutating motion of a spin-stabilized satellite. The equations of motion of the satellite-damper system are derived omitting consideration of the influence of external torques. The conditions of stability of the stationary spinning are obtained and the optimal parameters of the satellite and the damper ensuring a maximal rate of damping of the nutation motion are determined.     

Stellar mass loss in late B-type supergiants

A study using archive IUE data of time-varying mass loss has been carried out for a sample of 12 supergiants in the spectral range B5–B9. Additionally dedicated IUE velocity-time observations of discrete absorption components (DAC) in the UV resonance lines have been made for one of the stars (Ori), while optical data obtained for this star shows time variability in the H profile. Ions in which mass-loss features occur are unambiguously identified by comparing spectra of the stars at different mass loss episodes. Time variability in the mass-loss activity of late B-type supergiants is discussed and the stars are examined for trends with effective temperature. The basis for a theoretical model of the stellar wind in these stars is introduced.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain.     

Ускорение релятивистских электронов в плазменных реакторах и нелинейные спектры космических радиоисточников

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Повевхное магнитосферное течение С силяными разрывами

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Оболочки звездпри сверхкритической светимости

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О природе квазаров и активных ядер галактик

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, 40 48 MAC (, 1976).     

Перенос поляризации излучения В магнитоактивной космической плазме

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турбулентноштб в космологии

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Determination of the rotational excitation temperature in solar type stars

The OH molecular spectrum has been identified in three solar type stars, Com, CVn, and Cet. The rotational excitation temperature from molecular line intensities of OH has been determined for these stars. The observations in high resolution were made by use of the IUE satellite.Based on observations by the International Ultraviolet Explorer collected at the Villafranca Satellite Tracking Station of the European Space Agency.     

Энтропийны и АдиАъатические возмущения плотноти Маслого масщтаща — антивещество во вслэнной

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Statistical data analysis for gamma-ray astronomy

Significance testing, parameter estimation and sensitivity calculations for -ray telescopes are discussed for single on-off astronomical observations. Four widely used significance test methods are examined by Monte-Carlo simulations. The Maximum Likelihood Ratio Method is found to consistently over-estimate the significance of an observation by a few percents whereas the Fisher's Exact Test is shown to be slightly conservative and always under-estimates the significance by about the same amount when the reported significance is about 3 and therefore it is preferred for -ray astronomy applications. Two methods for constructing a confidence interval and an upper limit for -ray source counts are discussed. It is found that the method based on the Smooth Transformation provides slightly better estimations. A new formula for the calculation of the sensitivity of a -ray telescope is presented, in contrast to the widely accepted one, and their statistical meanings are explained in detail.