Cosmic-ray acceleration during the impact of shocks on dense clouds

Details Cosmic-ray acceleration during the impact of shocks on dense clouds Cosmic-ray acceleration during the impact of shocks on dense clouds

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...402..560j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 402, no. 2, p. 560-573.

Astronomy and Astrophysics

Astrophysics

44

Cosmic Rays, Dense Plasmas, Molecular Clouds, Particle Acceleration, Shock Waves, Bow Waves, Emissivity, Energetic Particles, Hydrodynamic Equations, Two Dimensional Models, Two Fluid Models

Scientific paper

In order to elucidate the properties of diffusive shock acceleration in nonuniform environments, an extensive set of simulations of the dynamical interactions between plane nonradiative shocks and dense gas clouds was carried out initially in static equilibrium with their environments. These time-dependent calculations are based on the two-fluid model for diffusive cosmic ray transport, and include the dynamically active energetic proton component of the cosmic rays as well as passive electron and magnetic field components. Except when the incident shock is itself already dominated by cosmic ray pressure, it is found that the presence of the cloud adds little to the net acceleration efficiency of the original shock and can, in fact, reduce slightly the net amount of energy transferred to cosmic rays after a given time. It is found that, in 2D cloud simulations, the always-weak bow shock and the shock inside the cloud are less important to acceleration during the interaction than the tail shock.

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