Instabilities in energetic particle modified shocks

Details Instabilities in energetic particle modified shocks Instabilities in energetic particle modified shocks

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...233..275z&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 233, no. 1, July 1990, p. 275-284.

Statistics

Computation

58

Computational Astrophysics, Cosmic Rays, Energetic Particles, Magnetohydrodynamic Stability, Shock Wave Propagation, Perturbation Theory, Relativistic Particles, Stellar Winds, Thermal Plasmas, Two Fluid Models

Scientific paper

The stability of obliquely propagating magnetosonic modes in the precursor or smoothed section of an oblique cosmic ray modified shock is considered. Three physical effects, which act through the gradient of the inhomogeneous flow, are identified as inducing either further wave damping or instabilities. The stability of waves in both parallel and perpendicular shocks is examined in detail and the role of strong, intermediate and weak cosmic ray scattering is explored. Several wave modes are found to be destabilized by one of, or a combination of, 'squeezing', 'stratification', and energetic particle drift. The implications for cosmic ray modified shocks, cosmic ray-modified galactic winds, and stellar wind termination shocks are discussed briefly.

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