Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...312..170j&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 312, Jan. 1, 1987, p. 170-177.
Astronomy and Astrophysics
Astrophysics
75
Cosmic Rays, Interstellar Magnetic Fields, Milky Way Galaxy, Shock Waves, Astronomical Models, Finite Difference Theory, High Energy Interactions, Iron, Particle Acceleration, Two Dimensional Flow
Scientific paper
Results are reported from numerical modeling of the acceleration and transport of ultra-high-energy cosmic rays in a galactic wind and its termination shock. A two-dimensional (azimuthally symmetric) wind and spiral magnetic field, with a spherical termination shock, where the velocity drops suddenly, is assumed. The time-dependent cosmic-ray transport equation, including all major transport effects is solved using an implicit finite-difference scheme. Particles are injected as the shock of low energy, and the subsequent evolution of the distribution function is followed. Iron nuclei are readily accelerated at the shock to energies up to 100 billion GeV, and protons to 10 billion GeV. A major effect aiding the acceleration of these particles is the spiral of the magnetic field carried out by the wind, caused by the rotation of the Galaxy, with the result that the shock is nearly normal over most of its area. Increasing the magnetic field or rotation rate increases the maximum energy attainable. Anisotropies and energy densities of the particles are also discussed. It is concluded that the process is consistent with observations of ultra-high-energy cosmic rays.
Jokipii Randy J.
Morfill Gregor
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