Abstract
Two specific regions of the magnetosphere are considered; (1) the magnetospheric tail, the region characterized by a sharp break of magnetic field lines at the neutral sheet, (i.e. lines that close an indefinite but large distance from the Earth) and (2) the magnetospheric core, the region with smooth closed lines of force. The maximum possible rate of magnetic field annihilation in the magnetospheric tail is estimated, using a hydrodynamic approximation and taking into account the anisotropy of the plasma pressure. This annihilation rate may be expressed in terms of an electric field which is directed from the morning side of the magnetosphere to the evening side. The motion of superthermal particles with the ‘one-particle approximation’ is also considered.
The magnetic drift shells in the magnetospheric core are calculated. In the outer distant regions of the core, the shells are split, according as the pitch angle of the particles is greater or smaller than a critical value, and form two branches, extending into the northern and southern hemisphere, respectively. The totality of the shells which intersect the boundary of the magnetospheric core constitutes the region of quasi-trapped particles.
One aspect of particle diffusion over magnetic shells (neglecting the splitting of shells) is also considered, that is, the shape of the stable distribution function for protons which is the stationary solution of the diffusion equation, without any losses. This case is actually realized beyond the intensity maximum of proton belt. Comparison with observation shows a sharp discrepancy between the observed profiles of proton intensity near the maximum of solar activity and those predicted by the generally accepted theory of diffusion. This discrepancy may be eliminated if one takes into account the effect of the gas pressure of trapped protons on particle motions over the shells (spontaneous convection), together with the effect of external forces in the form of electric fields and of azimuthally asymmetric pulses of the magnetic field (forced convection); for this, the relation of coefficients in the Fokker-Planck equation is essentially changed. The result is independent of the specific form of the diffusion coefficient. The above-mentioned problems have been considered in more detail elsewhere (Shabansky,1970).
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Shabansky, V.P. (1972). Particle Motions in the Earth’s Magnetosphere. In: Dyer, E.R. (eds) Solar-Terrestrial Physics/1970. Astrophysics and Space Science Library, vol 29. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3693-5_23
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DOI: https://doi.org/10.1007/978-94-009-3693-5_23
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