17 research outputs found
Formation of relativistic jets by collapsing stars to black holes
Formation of relativistic jets in the magnetosphere of collapsing stars is
considered. These jets will be formed in the polar caps of magnetosphere of
collapsing star, where the stellar magnetic field increases during the collapse
and the charged particles are accelerated. The jets will generate non-thermal
radiation. The analysis of dynamics and emission of particles in the stellar
magnetosphere under collapse shows that collapsing stars can by powerful
sources of relativistic jets.Comment: 8 pages, 3 figures, Accepted for publication in Adv. Space Re
Generation of high-energy particles, neutrino and fotons in magnetosphere of collapsing star
The generation of particles, photons and neutrinos in magnetosphere of collapsing star are considered. These processes are caused the self-interaction initial accelerating in magnetosphere protons and electrons. The second particles and photons will arise as a result of this self-interaction, which in turn will generate charged particles, photons and neutrino (cascade process). These processes are especially effective for the formation collapsing star magnetosphere from the secondary charged particles. In addition, the particles, photons and neutrinos will be generated in magnetosphere of collapsing star as result of these processes
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.