The evolution of cosmic-ray-mediated magnetohydrodynamic shocks: A two-fluid approach

Details The evolution of cosmic-ray-mediated magnetohydrodynamic shocks: A two-fluid approach The evolution of cosmic-ray-mediated magnetohydrodynamic shocks: A two-fluid approach

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...429..748j&link_type=abstract

The Astrophysical Journal, vol. 429, no. 2, pt. 1, p. 748-758

Computer Science

Numerical Analysis

7

Cosmic Rays, Efficiency, Evolution (Development), Kinematics, Magnetic Fields, Magnetohydrodynamics, Particle Acceleration, Shock Waves, Two Fluid Models, Viscosity, Analytic Functions, Numerical Analysis, Solutions, Steady State

Scientific paper

We study the shock structure and acceleration efficiency of cosmic-ray mediated Magnetohydrodynamic (MHD) shocks both analytically and numerically by using a two-fluid model. Our model includes the dynamical effect of magnetic fields and cosmic rays on a background thermal fluid. The steady state solution is derived by following the technique of Drury & Voelk (1981) and compared to numerical results. We explore the time evolution of plane-perpendicular, piston-driven shocks. From the results of analytical and numerical studies, we conclude that the mean magnetic field plays an important role in the structure and acceleration efficiency of cosmic-ray mediated MHD shocks. The acceleration of cosmic-ray particles becomes less efficient in the presence of strong magnetic pressure since the field makes the shock less compressive. This feature is more prominent at low Mach numbers than at high Mach numbers.

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