No abstract available

[en] Complete text of publication follows. Long term observations of loss of relativistic electrons to the atmosphere is presented and related to SW parameters. It is shown that the L-region of relativistic electron losses match the anisotropic proton zone. In this zone the pitch angle distribution of the protons are unstable and can generate/amplify EMIC waves, which in turn scatter the electrons into the atmosphere. In spatial limited regions, located close to the plasma pause, there can be enhanced losses of protons (sometime completely filling the loss cone). These regions of proton losses (spikes) are shown to give rise to EMIC waves leading to enhance scattering of the relativistic electrons. In the main phase of the storm the proton spikes are located in the midnight/evening sector, but in the storm recovery phase they are located at all MLTs. Proton spikes are observed in all storms, but loss of relativistic electrons only takes place in some storms.

[en] Complete text of publication follows. The precipitating protons play an important role in the heat budget of polar thermosphere during solar proton events. In this paper the proton heating efficiency is studied using all possible sources of heating and cooling of polar thermosphere. A special attention is paid on the reaction N₂(A³ EMBED Equation.3 ) + O which is considered as one of the most significant source of proton heating in auroral region. The new findings of temperature dependence of the reaction rate coefficient of the reaction N₂(A³ EMBED Equation.3 ) + O are also incorporated in the model. The proton heating efficiency is found as high as 71 percent in the peak energy deposition region (110-130 Km) and it strongly depends on altitude. These results would be very useful in the study of heat budget of polar thermosphere during solar proton events.

No abstract available

[en] Observations of a pulsed precipitation of protons with E/sub p/> or =12, 100, and 350 MeV on a high-altitude balloon are discussed. The relationship between these precipitation events and a pulsed disturbance of the magnetosphere is analyzed, as are possible precipitation mechanisms

No abstract available

[en] Observations of pulsating auroras in the magnetic zenith and proton and electron auroras along the magnetic meridian were conducted from three stations covering from 58⁰ to 71⁰ invariant during the pulsating aurora campaign in Saskatchewan in January and February of 1980. Pulsations were observed only south of or on the southern edge of the proton precipitation region. This is in general agreement with other uncoordinated studies of proton and pulsating auroras in the late morning hours, but it also appears to be true for isolated events at other times as well. (auth)

[en] The association between energetic protons (0.29--0.50 MeV) and simultaneous local fluctuations of magnetic field at 35 to 45 R_E in the magnetotail is examined statistically with data from APL/JHU particle telescopes aboard IMP 7 and IMP 8. About four satellite years of 5.5 min averaged measurements are used in this study. In addition to confirming that the level of magnetic field fluctuations generally increases with the presence of energetic protons and their streaming anisotropy, it is found that increase in occurrence frequency of streaming of energetic protons are ordered far better by magnetic field fluctuations (deltaB>5nT or deltaB/B>50%) is neither a neccessary nor a sufficient condition for the detection of large streaming in energetic protons

[en] The results of an experiment on the action of low-frequency radiation on the magnetospheric plasma are presented. Such action stimulates precipitation of protons. A preliminary interpretation of the data is given

[en] A mechanism for the interaction of fast protons with a VLF wave in the inhomogeneous magnetospheric plasma is proposed to explain the observed features of stimulated precipitation ]R. A. Kovrazhkin et al., Pis'ma Zh. Eksp. Teor. Fiz. 39, 193 (1984) [JETP Lett. 39, 228 (1984)]]