Ion Bernstein instability in the terrestrial magnetosphere: Linear dispersion theory

Details Ion Bernstein instability in the terrestrial magnetosphere: Linear dispersion theory Ion Bernstein instability in the terrestrial magnetosphere: Linear dispersion theory

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jgra..11512209g&link_type=abstract

Journal of Geophysical Research, Volume 115, Issue A12, CiteID A12209

Physics

Plasma Physics

7

Space Plasma Physics: Kinetic Waves And Instabilities, Magnetospheric Physics: Plasma Waves And Instabilities (2471)

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(ν$\perp$)/∂ν$\perp$ > 0, where $\perp$ denotes directions perpendicular to the background magnetic field Bo. Here fp(v) = f1(ν) - f2(ν), 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 ωr $\simeq$ nΩp, where n = 1, 2, 3, … and Ωp is the proton cyclotron frequency; wave vector k at 0 < k$\parallel$ $\ll$ k$\perp$, where $\parallel$ and $\perp$ 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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