Evolution of the fire-hose instability: Linear theory and wave-wave coupling

Details Evolution of the fire-hose instability: Linear theory and wave-wave coupling Evolution of the fire-hose instability: Linear theory and wave-wave coupling

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996jgr...10124457q&link_type=abstract

Journal of Geophysical Research, Volume 101, Issue A11, p. 24457-24470

Physics

Plasma Physics

24

Space Plasma Physics: Charged Particle Motion And Acceleration, Space Plasma Physics: Kinetic And Mhd Theory, Space Plasma Physics: Wave/Particle Interactions

Scientific paper

Large ion thermal or kinetic pressure anisotropies have been inferred to exist in conjunction with supernova shocks as well as in the solar wind/cometary interaction region and upstream from planetary bow shocks. For sufficiently strong thermal or beam-driven anisotropies, electromagnetic instability develops, isotropizing and scattering the ion populations. In particular, if the effective plasma β >2 (where β is the ratio of plasma pressure to magnetic pressure), and if the anisotropy is such that the temperature parallel to the magnetic field exceeds the perpendicular, then fire-hose instability can result, generating transverse magnetic field fluctuations. In high-β interstellar plasmas with large anisotropies, the level of the excited fluctuations may be quite large, exceeding even the ambient magnetic field. After a period of inverse-cascade to longer wavelengths, it may provide a potential source for the scattering of cosmic rays. In this study we simulate the evolution of the fire-hose instability using a standard one-dimensional hybrid code (macroparticle ions, massless fluid electrons). We find that the wave evolution proceeds in two stages. A rapid period of growth brings the plasma back to approximate marginal stability. There follows a second stage of slower evolution dominated by wave-wave interaction. During the second stage, the wave energy spectrum clearly exhibits an inverse cascade. Implications for cosmic ray scattering will be discussed.

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