Formation of the cosmic-ray spectrum due to its propagation in the Galaxy

A model of cosmic ray propagation is proposed to explain the knee of the cosmic ray energy spectrum in the energy range $E\sim 10^{14}{-} 10^{17}$ eV. The numerous stellar winds (SW), ionized hydrogen regions (H-II) and supernova remnants (SNR) in the Galaxy are taken into account in this model. The gas density and the magnetic field in these regions are different from the interstellar gas density and the interstellar magnetic field. Therefore they act as scattering centres and magnetic traps for cosmic rays. It is shown that these regions influence cosmic ray propagation in the Galaxy. Our results show that the collision time between cosmic rays and the SNR, SW, and H-II regions is much less than the cosmic ray lifetime in standard models (Berezinskii et al. 1984; Ginzburg & Syrovatskii 1963), in which only the nuclear interaction of the particles with interstellar gas is taken into account. Cosmic ray energies, and thus the cosmic ray spectrum, change due to interactions with these regions. Cosmic ray energy losses in these regions due to adiabatic cooling are comparable to the losses due to nuclear interaction with interstellar gas. It is therefore necessary to take these into account in galactic cosmic ray propagation models.

GRAVITATIONAL COLLAPSE OF STARS AND THE METHODS OF ITS OBSERVATIONS

It is present a review of the models of the later stages of stellar evolution and the mechanisms of the generation of neutrinos, charged particles and electromagnetic radiation during the gravitational collapse of stars. The conclusion was made that the most likely method for the registration of the gravitational collapse of stars is the registration of the nonthermal electromagnetic radiation generating in the magnetos

PARTICLES, NEUTRINO AND PHOTONS IN THE MAGNETOSPHERE OF A COLLAPSING STAR

The formation of the stellar magnetosphere during the gravitational collapse is discussed. Primary protons and electrons accelerate in the star’s magnetosphere during its gravitational collapse. In what follows, the flux of particles, photons and neutrinos generated in the magnetosphere is multiplied in a cascade process initiated by the self-interaction of particles and their interaction with magnetic fields. These processes are especially effective for the formation of magnetospheres in collapsing star