8 research outputs found
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 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