[en] The flux densities of Cassiopeia A radio emission are given in the scale based on absolute measurements by the method of ''artificial Moon''. The data of the present paper form the common evolutionary sequence of ''instantaneous'' spectra of 31-year duration, from 1953 through 1984, filled with an 1-2 year interval. The flux and the spectral index experience the ''secular'' decrease and oscillations with a 6-year period. The time and frequency dependences for these values have been obtained. The spectral index of the low-frequency region of the spectrum (<400 MHz) is smaller than that for higher frequencies and does not experience 6-year oscillations. The analysis of all published data on the rate of Cassiopeia A flux decrease is given

[en] A formation scenario for stringlike large-scale structure of the Universe is discussed. The main physical mechanism is the matter accretion into the wake of a rapidly moving massive body. The previously formed galaxy clusters and almost symmetric loops are considered as such bodies in the cases of the entropy model and the cosmic strings model respectively. Estimates indicate that, due to developing gravitational instability, the wake of the loop breaks into blobs with masses approaching those of the galaxies. Long-wave perturbations can cause the formation of protoclusters from these blobs of matter

[en] It is shown that accounting for anisotropy of X radiation from an accretion disk surrounding a black hole allows to achieve the agreement between the observed and theoretical optical light curves of the system LMC X-3. The restriction on the parameters of the LMC X-3 system and the mass of the X-ray object are obtained, and conclusion is drwan that the relativistic object in the system LMC X-3 is most probably a black hole

[en] It is shown that peculiarities of light and color variations observed at the time of deep minima of R CrB may be due to the variations of optical properties of particles when the size of particles at the time of circumstellar dust envelope formation. The dependence of the wavelength of extinction maximum of light on the particle size leads to the wavelength dependence of time delay of minima: the long-wave minima occur after short-wave minima. It results in color variations: the reddening at the decrease of light is replaced by the bluing at the minimum level of the star's brightness

[en] The results of UBV photoelectric photometry with different aperture sizes of the galaxies NGC 205 and M 33 are presented, including those obtained with small aperture sizes. The aperture decreasing, colour of NGC 205 chages first to blue and than to red: it is connected with the existence of a group of young stars in the central region of this galaxy. Colour of M 33, with approaching the centre, becomes a little bit redder. Properties of stellar-like nuclei of M 31, M 32, NGC 205 and M 33 are considered. Magnitudes and colours of the nuclei are shown to be different in the range of ΔV=3^m, Δ(B-V)=O^m,4 and Δ(U-B)=O^m,6. M 32 nucleus has the maximum luminosity and M 31 has the reddest nucleus. M 33 has the most blue nucleus

[en] The photoelectric observations in the vicinity of the He1 infrared line 10830 A were made with three solar instruments. Observations were made during some years in the period of the increase, maximum and decrease of the solar activity. Spectra have been registered many times both in active and in quiescent regions on the solar disc. A small depression in the short-wave wing of the telluric line 10832, 1 A is identified as due to solar ³He, blended by a small telluric line. After taking into consideration the telluric blends, an estimate was made of the abundance ratio ³He/⁴He for the observations of 1981 and 1985. It is shown that at the maximum solar activity, the abundance ratio in the spectrum of the normal chromosphere, probably, insignificantly increases

[en] The methods of restoration of radial brightness distribution across a stellar disk from an anaysis of speckle interferometric data in the case of circular symmetry are proposed. These methods are based on modern numerical methods of solution of ill-posed problems. The application of these methods to an analysis of published data for α Ori allows to find the brightness distributions for the TiO absorption band and the neighbouring continuum. The results do not contradict the assumption that this star has a near-by dust envelope located inside the extended atmosphere

[en] Among the absorption lines of L_α forest in the spectrum of the QCD S5 0014+81, there is a unique phenomenon of 8 strong Lyman lines, five of which are observed as double ones with practically identical equivalent widths for each pair and with the same velocity splitting Δλ/λ for all the system. This phenomenon can be naturally explained within the framework of the model of the L_α forest as absorbing zones in the shells of metagalactic shock waves. Main features of the ''twin'' absorption systems in the spectrum of S5 0014+81 are explained both qualitatively and quantitatively, if the line of sight lies near the edge of the shock-wave shell. This specific geometry opens favourable opportunities for the search for weaker lines of metals. Helium and deuterim; their detection in the QCD spectrum would be of great importance for both cosmology and cosmogony. In the appendix some analytical expressions related to density distribution behind the strong adiabatic cosmological shock wave, which make possible to use numerical computations for other cosmological epochs are given

[en] The factors influencing the star formation in the inner regions of Seyfert galaxies are considered. The UV and X-ray radiation of the galactic nucleus with the luminosity L_ion >or approx. 10⁴⁴ erg/s results in the disruption of molecular clouds in the inner zone with the radius >or approx. 0.1 kpc during the time t=10⁷ yr. It is shown that the outflow from the nucleus results in the transport of mass 10⁷-10⁸ M_sun into the inner zone with the radius 0.5-1 kpc. Under the decrease of nuclear luminocity with time, the gas may be a mass resource for the star formation

[en] The carbon abundance was obtained for 38 single stars and 48 brighter components of binary stars on the basis of high-dispersion data for carbon line widths. The LTE (for C II lines) and non-LTE (for C III lines) approach was applied. The mean value of lg N(C) is 8.5+0.3 for the single stars and 8.3±0.3 for the binary ones. The lesser carbon abundance for the binaries may be explained by a more intense transfer of CNO-cycle products from the central parts of the stars to their surface layers than for the single stars