Ion Bernstein Instability in the Magnetosphere: Linear Dispersion Theory

Details Ion Bernstein Instability in the Magnetosphere: Linear Dispersion Theory Ion Bernstein Instability in the Magnetosphere: Linear Dispersion Theory

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm11b1721g&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM11B-1721

Physics

Plasma Physics

[2772] Magnetospheric Physics / Plasma Waves And Instabilities, [7829] Space Plasma Physics / Kinetic Waves And Instabilities

Scientific paper

Linear kinetic dispersion theory for electromagnetic fluctuations in a homogeneous, magnetized, collisionless plasma is used to study the properties of an ion Bernstein mode instability driven by a proton velocity distribution fp( v) such that ∂ fp(v⊥)/∂ v⊥ > 0 where ⊥ denotes directions perpendicular to the background magnetic field Bo. Here fp( v) = f1(v) -f2(v) where f1 and f2 are Maxwellian velocity distributions with slightly different densities and temperatures; plasma parameters are taken from magnetospheric observations. Then the growth rate of this instability has relative maxima at the fundamental and harmonics of ω r ≃ Ω p, the proton cyclotron frequency, wavevector k at 0 < k∥ << k⊥ where ∥ and ⊥ denote the directions parallel and perpendicular to Bo, and wavelengths of the order of or smaller than the proton gyroradius. The maximum instability growth rate is a monotonically decreasing function of the electron-to-proton temperature ratio, but has its largest value at an intermediate value of the proton β ( ˜ 0.5 for the parameters considered here).

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