Weak pitch angle scattering of energetic protons in the magnetosphere

Details Weak pitch angle scattering of energetic protons in the magnetosphere Weak pitch angle scattering of energetic protons in the magnetosphere

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975jgr....80.2745s&link_type=abstract

Journal of Geophysical Research, vol. 80, July 1, 1975, p. 2745-2750.

Physics

1

Earth Magnetosphere, Proton Scattering, Solar Flares, Solar Protons, Angular Distribution, Geomagnetic Tail, Magnetohydrodynamic Waves, Pitch (Inclination), Proton Energy, Proton Flux Density, Resonant Frequencies, Trapped Particles

Scientific paper

During the solar particle event of April 12-14, 1973, a flux depression of solar protons in the dawn side pseudotrapping region relative to the flux in the dusk side pseudotrapping region was frequently observed with the low-altitude polar-orbiting satellite ESRO 4. This flux decrease is interpreted as being due to weak pitch angle scattering of the solar protons during their drift from dusk to dawn. Treating the pitch angle diffusion as a simple initial value problem, we derive quantitative values of the equatorial bounce-averaged pitch angle diffusion coefficients at small pitch angles for different energies. These values represent lower limits for magnetospheric conditions at the time of the ESRO 4 observations. Through the assumption that the pitch angle diffusion is a gyroresonant interaction process of the particles with either Alfven or ion cyclotron waves, the necessary power of the waves at the resonant interaction frequency is calculated.

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