εлектроны космических лучей радиогало галактики

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Микрофлуктуации электрического поля на фронте ударной волны в модельном эксперименте

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Non-restricted double-averaged three body problem in Hill's case

A limiting case of the problem of three bodies (m ₀,m ₁,m ₂) is considered. The distance between the bodiesm ₀ andm ₁ is assumed to be much less than that between their barycenter and the bodym ₂ so that one may use Hill's approximation for the potential of interaction between the bodiesm ₁ andm ₂. In the absence of resonant relations the potential, double-averaged by the mean longitudes ofm ₁ andm ₂, describes the secular evolution of the orbits in the first approximation of the perturbation theory.As Harrington has shown, this problem is integrable. In the present paper a qualitative investigation of the evolution of the orbits and comparison with the analogous case in the restricted problem are carried out.The set of initial data is found, for which a collision between the bodiesm ₀ andm ₁ takes place.The region of the parameters of the problem is determined, for which plane retrograde motion is unstable.In a special example the results of approximate analysis are compared with those of numerical integration of the exact equations of the three body problem.

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m ₀,m ₁,m ₂. , m ₀ m ₁. m ₂, m ₁ m ₂ m ₁ m ₂ . , . . , m ₀ m ₁. , . .

     

Динамические равновесные плазменные конфигуации и физика магнитосферы

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О колебаниях хвоста магнитосферы в приБлижении квазигидро динамики

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Возможный механизм радиоизлучения пульсаров

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The distribution of the angular momenta of galaxies

Since the average relation between the angular momentaP and the massesM of galaxies can be represented by a power lawPM , we can define a relative angular momentum =P/M (or a constant timeP/M ). For a random motion picture within protogalaxies, should follow a Maxwellian distribution and consequently the dispersion of log should be 0.210.For the reasonable range of ( to 2), the limited sample of galaxies with known dynamical parameters gives between and 1 times the Maxwellian value. For the plausible special case =2 the reciprocal of the maximum rotational velocityv _m is already a measure of and the larger sample ofv _m-values not only yields the Maxwellian but, moreover, shows the shape of the distribution.

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PM , =constP/M . , (lg )=0.210. 7/42, . =2 v _m- .

     

Critical inclinations in planetary problems

The general conception of the critical inclinations and eccentricities for theN-planet problem is introduced. The connection of this conception with the existence and stability of particular solutions is established. In the restricted circular problem of three bodies the existence of the critical inclinations is proved for any values of the ratio of semiaxes . The asymptotic behaviour of the critical inclinations as 1 is investigated.

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Взаимодействие вещества и излучения В Горячей модели вселенной

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In this paper we continue the work of Weymann, investigating the causes of distortion of the spectrum of the residual radiation from the Planck curve. We discuss the distortion to the spectrum, resulting from recombination of primeval plasma.We then derive an analytic expression for the distortion to the equilibrium spectrum due to Compton scattering by hot electrons. On the basis of the observational data we conclude that a period of the existence of neutral hydrogen is inescapable in the hot model of the universe. It is concluded that any injection of energy att>10¹⁰ sec (red shiftz<10⁵) give the distortions of the equilibrium spectrum.

     

A study of the young open cluster NGC 6611

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Радиоизлучение Быстрых космических ионов

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Повевхное магнитосферное течение С силяными разрывами

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Структура Области Взаимодействия Солнечного Ветра С Межзвездной Средой и Ее Влияние На Проникновение Атомов Н в Солнечный Ветер

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Литосфера Луны По Данным Электромагнитного Зондирования

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Observation of far ultraviolet radiation from early-type stars

Rocket-borne photon counters sensitive to bands 1060–1180, 1230–1350, and 1350–1480 were used to measure the celestial ultraviolet radiation above the terrestrial atmosphere. The energy spectra of six objects, Leo, CMa, Ori, , , Ori (combined), Ori, and Tau were obtained. The comparison of them with those calculated with the stellar model atmospheres indicates the deficiency of about 1 mag. in the ultraviolet region, when corrected for interstellar extinction, for all stars except Tau. The observed spectrum of Tau agreed with the theoretical one for normal interstellar extinction. The effects of line blanketing were examined for B1 and B2 stars, and found to account for a part of the difference between the observed and the theoretical values.     

Слектры релятивистских эиектронов и изиучения, формируемьЫе комптоновским рассеянием лри отличном от нуля потоке

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НутационнЫе демпферы спутиков С двойным вращением

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Nutational dampers of dual-spin satellites

The paper considers application of the small parameter methods (Artemjev, 1944; Volosov, 1962) in the linear theory of damping the nutating motion of dual-spin satellites. The external moments affecting the satellite are left out of consideration. The influence of the damper on the satellite motion is assumed to be small. As a special case the conditions of stability for the satellite stationary spinning and the optimal parameters ensuring a maximal rate of damping the nutating motion have been obtained.

     

Sur les solutions Lagrangiennes et euleriennes du probleme generalise des trois corps en axes absolus

Résumé Le présent travail est une continuation d'un autre, publié plus tôt (Doubochine, 1970). On montre ici, que les propriétés des mouvements Lagrangiens et Euleriens établies en mécanique céleste classique sont vraies aussi dans les cas plus généraux, envisagés dans le travail indiqué. On montre de plus, que les trajectoires des points en ces mouvements en axes absolus sont les spirales infinies s'enroulant sur les surfaces des cylindres curvilignes infinis.

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Sur le probleme restreint circulaire des trois corps solides

Résumé Il est envisagé dans ce travail un cas particulier du problème des trois corps solides. On suppose qu'un des corps est passif, c'est-à-dire qu'il n'agit pas sur les deux autres. Chaque corps posséde la symétrie axiale, ainsi que la symétrie par rapport à plan, perpendiculaire à cet axe, Au moment initial les plans de la symétrie des corps coinsident avec le plan principal des coordonneés. Alors il est possible de choisir les conditions initiales de sorte que les centres de la symétrie resterons toujours dans le plan principal, chaque corps tournant uniformement autour son axe. Nous nommerons ce problème — le problème restreint plant. Le cas le plus simple est le problème plan circulire, quand le centre d'un des corps actif décrit orbite circulaire authour d'autre corps actif. Ce problème se reduit à l'étude du mouvement du centre d'inértie du corps passif dans le plan principal —plan d'orbite circulaire du corps actif. Nous trouvons les conditions d'existence pour les solutions particulières du ce problème et posons la question de la stabilité des points de libration correspondantes. D'une manière plus détaillée nous envisageons le cas, où toutes les forces actives sont définiérs une par loi unique.

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ЗйлеровьI рещения задчи о поступательно вращатльном движени трех твердьени трех твердьх тел

I I (, 1976). I :I I I I I I I (I) I I . I . , I I .

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Euler solutions in the problem of the translatory-rotary motion of three rigid bodies

The present paper is a continuation of the article (Vidyakin, 1976) in which we proved the existence of Lagrange (triangle) solutions in the general problem of the translatory-rotary motion of three absolutely rigid bodies.In particular, we have found the conditions for the existence of Lagrange solutions in the case when all the bodies possess a symmetry with respect to three mutually perpendicular planes both in respect to the distribution of matter and in respect to the outward form. In this case the bodies effect simple translations along with the centres of the masses without rotation (in Lyapunov's system of coordinates).If the rigid bodies possess a symmetry in respect to the axis and to the plane, perpendicular to this axis, then the Lagrange solutions of the three floats (Duboshin, 1973), three spokes (Kondurar, 1974), three shafts (Vidyakin, 1976) types are admitted, as well as the solutions in the cases of combinations of the float, spoke and shaft-bodies (Vidyakin, 1976).Those solutions exist of certain conditions, imposed on the structure, orientation and rotation of the bodies, are observed.In the general case (there) exist particular solutions which we have termed as Near-Lagrangian.The present paper is to prove the existence of Euler (rectilinear) solutions in the problem of the translatory-rotary motion of three rigid bodies, assuming that the elementary particles of the rigid bodies are mutually attracted according to the Newtonian law.In particular, we have found the conditions for the existence of Euler solutions in the case when all the bodies possess a symmetry in respect to three mutually perpendicular planes both in respect to the distribution of matter and in respect to the outward form. In this case the bodies are so disposed in the uniformly rotating coordinate system that two symmetry planes concur while the centres of the masses are disposed on one straight line.In particular, if the bodies possess a symmetry in respect to the axis and to the plane perpendicular to this axis, then the Euler solutions of the three floats (Duboshin, 1973), three spokes, three shafts types as well as solutions in the cases of combinations of float-, spoke- and shaft-bodies and spheres, either homogeneous or possessing a spherically symmetric distribution of densities, are admitted.The paper gives exact solutions for the cases when the attraction force function of the bodies has an approximate expression.