[en] Helium burning kinetics in white dwarfs has been considered at constant temperatures T >= 10⁹ K and densities rho >10⁵ g/cm³. It is found, that helium detonation in white dwarfs does not lead to formation of light (A < 56) elements. Thus, helium white dwarf model for supernova 1 is inconsistent with observations

No abstract available

[en] The oscillations arising at close encounters of stars is considered with the aid of numerical methods in linear adiabatic approximations. It is shown that two types of oscillatory motions appear due to the action of tidal force. The first one is normal mode described by spherical harmonic of degree l=2 and of order m=0. The second more important type of oscillation, with a several times higher amplitude is a running wave, propagating in the direction of parabolic motion of disturbing star. It is suggested that the 160-min oscillation of the Sun can be a relict phenomenon of encounter of the Sun with a low-mass star, or a cloud, at the earlier stage of solar evolution. It is also pointed out that the oscillations arising at close encounters are very similar to those of β Cephei stars

[en] Taking into account peculiar velocities of neutrinos the gaseous component is shown to dominate in the central part of a cosmological ''pancake'' (rhosub(p) > rhosub(ν)), while on the average anti rhosub(b) << anti rhosub(ν). Therefore fragmentation of a gaseous ''pancake'' and later clustering of the fragments into galaxies and groups of galaxies are determined by velocity distribution and gravity of the gaseous component. The hidden mass is formed by capture of neutrinos by clustering clouds. Formation of the cluster of galaxies is connected with perturbations embracing all the neutrino-gaseous ''pancake'', initial ratio of neutrino-to-gaseous densities being reestablished. It is shown that the first ''pancakes'' were formed at the red shifts z=5-8

[en] Limits for the magnitude of Solar oblateness under the assumption that the Sun is rotating as a rigid body with the velocity of sideric rotation of the equator points have been determined. It is demonstrated that for the present there is no necessity to take into accoUnt Solar oblateness when making the interior planets movement theories

[en] Oscillation regimes of cyclotron instability in the Jovian radiation belts are investigated. Essentially, the eigenfrequencies of these oscillations in the external Jovian magnetosphere do not depend on the magnetic shell and coincide with the rotation velocity of the planet. This gives an account of the ten-hour modulation of energetic electron fluxes, which was observed experimentally

[en] The absorption lines C638α-C641α are detected at 25 MHz in the region with galactic coordinates l₂=75 deg; b₂=0 deg and near the NGC 2024 nebulae. The observed parameters of lines can be only explained in the frame of the low-temperature dielectronic recombination mechanism. The advantages of decametric observations of carbon recombination lines in the various components of the interstellar medium are pointed out

[en] Some results are analysed of previoUs spectroscopic investigation of the supergiant HDE 226868 (based on six-year observations at the 6-m telescope) with the puspose of searching for possible variations in the spectrum connected with the precession of the rotation axis of the star upper layers. It is noted that spectral type and HeI lambda 4471 line halfwidth show a coordinated behaviour with the phase of the 39-day period in the frame of the precession hypothesis. Nonuniform distribution of CNO anomalies over the star latitude seems to be possible

[en] Normalized Stokes parameters of polarized radiation for ten observed cepheids are shown to occupy on the psub(x)-- psub(y)-plane the rosetteshaped regions having three pro ections. The interstellar component radius-vector for cepheids with interstellar polarization derived from observations of neighbourhood stars (Z Lac, VX Per) ends close to the base of ''rosette''. In the case of absence of interstellar polarization (W Vir, RR Lyr) the base of the ''rosette'' is located near the origin of coordinates. By analogy with these cases it is assumed that for other cepheids also the value of interstellar polarization can be derived from the position of the base of the ''rosette''. The directions of the interstellar polarization planes thus obtained turn out to be close to the directions of the large-scale magnetic field of the Galaxy

[en] Photometric UBVRJHK observations of the symbiotic star AS 296 are presented. No light valiations exceeding 0sup(m).2 are found. The cool star is classified as M5III. The color excegss is E(B-V)=sup(m).43+-0sup(m).04. Analysis of the photometric and spectral observations has shown that AS 296 is similar to V1016 Cyg at the moment of low brightness of the hot source. The luminosity of the hot component of AS 296 amounts up to approximately 200 Lsub(Sun) if provided its distance to be 2.2 kpc