[en] This book presents a discussion of aspects of the theory of particle transport in interplanetary space. Topics covered include solar wind, its magnetic field and structure, irregular magnetic fields, application to solar particles, shock acceleration, and modulation of galactic cosmic rays

No abstract available

[en] A variety of the avaiable observational data on the cosmic ray (CR) spectrum, anisotropy and composition are in good agreement with a suggestion on the diffusion propagation of CR with energy below 10(15) eV in the interstellar medium. The magnitude of the CR diffusion coefficient and its energy dependence are determined by interstellar medium (ISM) magnetic field spectra. Direct observational data on magnetic field spectra are still absent. A theoretical model to the turbulence generation in the multiphase ISM is resented. The model is based on the multiple generation of secondary shocks and concomitant large-scale rarefactions due to supernova shock interactions with interstellar clouds. The distribution function for ISM shocks are derived to include supernova statistics, diffuse cloud distribution, and various shock wave propagation regimes. This permits calculation of the ISM magnetic field fluctuation spectrum and CR diffusion coefficient for the hot phase of ISM

[en] Equations are derived in the WKB approximation describing the evolution of wave vectors, polarization and amplitudes of magnetosonic and Alfven waves in a nonuniform moving medium. Results of general theory are applied to the propagation of magnetohydrodynamic waves in the solar wind plasma. The results of this examination are in qualitative agreement with the observed data on anisotropy of the Alfven wave spectrum in the solar wind. 18 refs

[en] Short note

[en] Briefly reviewed are the main processes of fast particle interaction with the shock front, namely the relative role of the Fermi acceleration the acceleration by the regular electric field of the shock wave, and also the reflection of particles from the shock front. The equations and the boundary conditions for the phase density of particles in the shock front are derived. These equations provide for a strict formulation of the problems of particle transfer and acceleration in the turbulent medium in the presence of sharp shock fronts, as well as of rarefaction waves and other large-scale disturbances. The solutions of this problem for a few simplest onedimensional cases are presented. The problem of the formation of the accelerated particle spectra in the interplanetary space and in the supernovae remnants, including the formation of the power-like spectra with weak dependence on the detailed mechanism of acceleration, is discussed. Some possible manifestations of the acceleration mechanism considered in galactic and extra-galactic radio-sources are pointed out

[en] The solution of a non-stationary problem on particle acceleration by shock wave in a turbulent interplanet medium is observed in a one-dimensional model. The shock waVe in the turbulent medium can accelerate particles in the result of three factor effect: 1) regular electric field of the shock wave; 2) mermiev acceleration with magnetic non-uniformities, which move at different rates in front and behind the front; 3) particle acceleration by turbulence behind the front, which can be generated or noticeably strengthened by the shock wave. The particles are considered energetic enough, so that their larmor radius is large in comparison with the front thickness. The particle distribution function is supposed to be close to the isotropic one; a transfer equation is used for describing their movement. The processes of particle interation with the front (acceleration, reflection or conduction) are taken into account by the limiting condition, imposed on the particle concentrations and fluxes. Considered have been momentary particle injection and different dependences of the diffusion coefficient on the energy. Evaluated are the acceleration time and maxial energy of the particles, as well as their energy spectra. Comparison with the observation data shows, that many cases of intensity growth of fast particles, correlated with the shock wave coming, can be explained by particle acceleration by the shock wave

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No abstract available

[en] The effect of various modes of plasma turbulence (i.e. electron density fluctuations and small-scale magnetic and electric fields) on spectra of synchrotron radiation of relativistic particles is examined. It is shown that some features in the spectra of several cosmic objects may be explained by plasma mechanisms