[en] In the spectrum of the Venus night airglow eight bright bands have been observed in the range of wavelengths from 3900 to 6500 A. An attempt has been made to interpret this spectrum. Carbon monoxide CO should be the most wide spread biatomic molecule in the Venus upper atmosphere. The band positions calculated of the CO fourth positive system for the difference of the oscillation numbers ΔV=20-28 have been compared with the maxima of the bands observed. In all the cases the deviation does not exceed the spectrometer resolution. The bands of the Venus night airglow present sequents each corresponding to the constant difference of the oscillatory numbers of lower and upper electron states

[en] Deuterium role in the elementary processes of the Universe is investigated. The deuterium was formed during the ''Great explosion''. The modern deuterium amount should not be higher than the amount of the initial deuterium. Deuterium is not found on the Sun and other stars as it burns quickly there. On the Earth 1 ton of sea water contains 17 g of deuterium. Cosmic rays contain 100 times more deuterium than the Earth, while in the atmospheres of giants this amount is 3 times lower. There is one deuterium atom per 50000 hydrogen atom in the interstellar gas. According to the data of observations on interstellar molecules, there is one deuterium atom per 10-1000 hydrogen atoms. However, measurements of interstellar molecules can not be as reliable estimates of the real amount of deuterium in the interstellar medium. Results of measuring the DI/HI ratio, obtained according to absorption lines of atomic hydrogen are most reliable. The deuterium amount measured can be used to determine the mean density of the Universe and, consequently, the law of its expansion. The mean density of the matter in the Universe determined according to the deuterium amount and that actually observed in galaxies can be considered coinciding in the first approximation

[en] Angular distribution of OH absorption was measured in the galactic sources W3, W12, W41, W43, and AMWW52 (G 32.8 + 0.2) with the Nancay Radio Telescope. The beamwidth was 3.sup(')4xOne-dimensional distribution of the optical depth was obtained for 4 sources, and a two-dimensional distribution of the absorption was measured for W 43. The distributions show complex kinematic and angular structure as a result of absorption by both extended and compact gas clouds. The latter seem to be physically associated with H 2 regions and molecular maser sources. A new candidate to the compact gas clouds associated with supernova remnants and Class 2a 1720 MHz maser sources was found in W 41

[en] The ²¹Ne, ³⁶S, ³⁷Cl, ⁴⁰Ar, ⁴⁰K isotope production by the standard s-process is calculated so as to fit the abundances of elements heavier than iron observed in the solar system. A radioactive ⁴⁰K age of 6.7(+0.5, -0.6) x 10⁹ yr is obtained for single-event nucleosynthesis or (10.3 +- 2.0) x 10⁹ yr for continuous, constant-rate nucleosynthesis, in agreement with the ages of the r-process elements uranium and thorium as well as with the age of the iron in the Galaxy

No abstract available

[en] Spectra of H₂O maser sources obtained in the band 9 MHz (radial velocity range 120 km/s) in the first observations using acousto-optical 1008-channel radio spectpometer are presented. FluX Variability of spectral features was found within the time intervals from 75 days to 7 years

No abstract available

[en] Scientific problems which can be solved with the Earth-Space interferometer having a space ratio telescope 10 m in diameter in an elongated orbit with the height of the apogee 77000 km and the period of revolution 24 h are described. It operates together with ground-based telescopes in very long baseline interferometer mode. The angular resolution and sensitivity of this new kind of instrument will be sufficient for obtaining fundamental information about fine structure and physical nature of radio emitting regions adjacent to the environs of black holes, neutron stars and star forming regions

[en] Attempts to observe effects of absorption of background decameter radiation (at ß = 14.7, 16.7, 20 MHz) by Heiles' Cloud 2 place upper limits of roughly-equal10^-₂ cm^-₆ pc on its emission measure and roughly-equal10^-₁ cm^-₃ on its electron density

[en] A survey of 14 SNR's in the 4.8 GHz absorption line of H₂CO shows that two of them, W28 and W44, possibly interact with molecular clouds. The interaction leads to acceleration of a part of the molceular cloud to a velocity of approximately 5 km s^-1 without a significant increase in the kinetic temperature or turbulence. The apparent long-term stability of galactic molecular clouds against gravitational collapse and subsequent star formation has stimulated proposals about possible sources of external pressure, such as shocks, which could upset this equilibrium and lead to collapse. The supernova blast wave was considered as such a shock by Herbst and Assousa (1977). This proposal can be tested by observations. The interaction between a SNR and a molecular cloud may result in a disturbance of the cloud such as changing of its geometry, introducing large velocity gradients, heating etc. Spectral line mapping of the molecular clouds toward SNR's might reveal cases of SNR-molecular cloud interactions and give details of the relevant physical processes. The observations presented were aimed at (i) a search for clouds interacting with SNR's; (ii) measuring physical parameters of the disturbed molecular gas. (Auth.)