Instability of the structure of strong oblique MHD cosmic-ray shocks

Details Instability of the structure of strong oblique MHD cosmic-ray shocks Instability of the structure of strong oblique MHD cosmic-ray shocks

Oct 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ap%26ss.148..175c&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 148, no. 1, Oct. 1988, p. 175-187.

Statistics

Computation

10

Cosmic Plasma, Cosmic Rays, Magnetohydrodynamic Stability, Oblique Shock Waves, Thermal Plasmas, Computational Astrophysics, Interstellar Magnetic Fields, Particle Acceleration, Perturbation Theory, Plasma Diffusion, Radiation Pressure

Scientific paper

A criterion of the instability of a flow of a thermal plasma and cosmic rays in front of an oblique MHD shock wave with respect to short-wavelength magnetosonic disturbances is derived. The dependence of a cosmic-ray diffusion tensor on a plasma density and a large-scale magnetic field is taken into account. The most unstable disturbances propagate at an angle to the magnetic field if diffusion is strongly anisotropic. In some cases the most strong instability connects with the off-diagonal terms of the diffusion tensor.

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