V. N. Zirakashvili

TL;DR: The physical processes involved in diffusion of Galactic cosmic rays in the interstellar medium are addressed in this article, where the effect of wave dissipation has been incorporated in the GALPROP numerical propagation code in order to asses the impact on measurable astrophysical data.

TL;DR: In this article, the shape of the galactic cosmic rays (CR) diffusion coefficient was found to explain the observed peaks of secondary to primary nuclei ratios at a few GeV/n, and the dissipation of waves due to the resonant interaction with energetic particles may terminate the cascade at less than 1.e13 cm.

TL;DR: In this paper, the authors derived exact asymptotic solutions of the kinetic equation which describes the energy distribution of relativistic electrons formed via diffusive shock acceleration accompanied by intense nonthermal emission through synchrotron radiation and inverse Compton scattering.

TL;DR: In this article, a new numerical code was designed for the detailed numerical treatment of nonlinear diffusive shock acceleration, which is used for the modeling of particle acceleration and radiation in young supernova remnants (SNRs).

TL;DR: In this article, the authors show that the maximum energy of the accelerated particles strongly depends on the age of a SNR and that the average spectrum of cosmic rays injected in the interstellar medium in the course of the adiabatic SNR evolution (the Sedov stage) is approximately Q(p)p 2 ∝ p −2 at energies larger than 10−30 GeV/nucleon and with a maximum particle energy that is close to the position of the knee in the cosmic-ray spectrum observed at ∼4 × 10 15 eV.