[en] The main features of the method of combined wave diagnostics using the BUDVAR complex are presented. Examples of measurements on near-earth shock waves are given and the first results of a physical interpretation of processes taking place in the near-earth shock wave front are presented

[en] The results of measurements of the energy spectra and pitch-angle distributions of electrons with energies of 0.3-2.0 MeV in the inner belt, which were made on the Interkosmos-19 satellite in 1979, have been used to calculate the distribution function for constant values of the first and second adiabatic invariants. The shape of the distribution function indicates radial diffusion from an external source. The diffusion coefficient in the inner belt at L = 1.2-1.4 is determined from the radial diffusion equation

[en] We present the results of measurements of the three components of the magnetic field and of charged particle fluxes with 0.4 ≥ E ≥ 15 keV. The measurements were made simultaneously on board Interkosmos-Bolgariya-1300 in the daytime sector of local geomagnetic time. To determine the position of the cusp, we used spectral characteristics of the charged particles reaching the ionosphere. We investigate how the characteristics of the longitudinal currents in the cusp (determined from the magnetic measurements) are related to the IMF orientation. We investigate the asymmetry of the longitudinal currents in the northern and southern polar cusps. We have discovered intense small-scale currents in the cusp which are accompanied by abrupt enhancements in the flux of charged particles

[en] In January 1976, the Interplanetary Magnetospheric Study (IMS) began. During the period January-March 1976, geomagnetic disturbances coincided mainly with a recurring sequence of earth passages through sector structures in the interplanetary magnetic field (IMF). In March, unusually large enhancements in energetic electron fluxes were recorded by Prognoz 4. The observations were made during intersections of the flanks of the transition region (TR) in conditions of enhanced geomagnetic activity, and the enhancements were of significant duration. Intense bursts of these particles were also observed in the outer magnetosphere at high latitudes. We discuss possible mechanisms for creating such formations

[en] The characteristics of the solar wind and of the interplanetary magnetic field are investigated from April 3, 1968 to April 22, 1968. Two high-velocity solar wind streams occurred in this period; however, groundbased cosmic ray stations recorded only one ordinary Forbush effect from April 5 to April 7 and a slow restoration of the intensity until April 20. The modulation efficiency of two successive disturbances of the interplanetary medium is compared. Solar activity data have been drawn on for the analysis. An approximation for the intensity of cosmic rays has been obtained with parameters of the interplanetary medium and of solar activity

[en] The series of dual-frequency radio occultation experiments conducted in 1983-1984 with the Venera 15 and 16 satellites made it possible to determine characteristics of the dayside Venusian atmosphere during intermediate states of solar activity. A comparison of these data with similar results from the Venera 9 and 10 satellites clarifies a number of peculiarities in the behavior of the ionosphere that are related to the phase of the solar activity

[en] Dual-frequency radiographic experiments conducted with the Venera 15 and 16 satellites made it possible to obtain about 60 height profiles for electron density on the nightside of the planet. Data is presented that illustrates the high space-time variability of the ionosphere, which makes the detection of regularities in its behavior difficult. A comparative analysis between the data from Venera 15 and 16 and that from Venera 9 and 10 and Pioneer-Venera indicates that the characteristics of the height profiles of the electron density vary with the phase of the eleven-year cycle of solar activity. Numerical modeling of the experiment is used to determine the sensitivity of the dual-frequency radiographic method for investigating the upper nightside Venusian ionosphere

[en] The solar wind flow around Venus is modeled numerically, with loading of the flux by heavy ions formed by photoionization of the neutral oxygen corona of Venus taken into account. It is shown that this effect can explain a whole series of features of the interaction of the solar wind with the planet, which had yet to be explained unambiguously, viz., the position of the shock wave, the characteristics of the solar wind flux, and the magnetic field behind the front

[en] It is shown within the scope of the precessional dynamo model that satellites of the moon, which, as has been proposed, existed in equatorial orbits 4-3.8 Gyr ago and whose fall to the surface relates to the formation of the maria (14) and a change in position of the axis of rotation of the moon (15), could have determined the generation of a strong dynamo field of 10^-4 T in which the ancient lunar rocks acquired thermoremanent magnetization. The strong dynamo field attenuated with the fall of the satellites to the surface of the moon, but a moderate dynamo field could have been generated with the precession of the moon under the perturbing effect of the gravitational field of the earth. This field also attenuated with the recession of the moon from the earth and its acquisition of synchronous rotation. If the distribution of the paleofields over the entire surface of the moon, which one can hope will be established, confirms the assumption of uniform magnetization of the lunar crest by a field of internal origin, then the planetary precessional dynamo model gets additional proof of the established cause-effect relation: If the source inducing the precessional motion disappears, then the magnetic field disappears

[en] The article examines properties of the day and night ionosphere of Venus and some possible sources of its ionization and discusses the disagreement of measurement results in different experiments with automatic stations and the results of observations of the upper ionosphere by radio-occultation methods. It is shown that there has not yet been achieved a satisfactory quantitative description of the Venusian ionosphere on the whole