Convective Injection of Energetic Radiation Belt Electrons Contrasted with Diffusive Loss in the Outer Zone: the Net Effect of Radial Transport

Physics

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2720 Energetic Particles: Trapped, 2730 Magnetosphere: Inner, 2760 Plasma Convection (2463), 2764 Plasma Sheet, 2774 Radiation Belts

Scientific paper

Energetic electron fluxes in the outer radiation belts vary as a result of a complex balance between transport, acceleration, and loss. Quantifying these variations will require a thorough understanding of the physics and characteristics of the individual processes independently acting on the radiation belts. Radial transport, in which particles conserving the gyro invariant move through regions of varying magnetic field strength, may lead to heating as particles move into regions of stronger magnetic field, or may contribute to the loss of radiation belt particles by transport out of the trapping region and through the magnetopause. In this work we use MHD/particle simulations to examine the net effect of radial transport in the radiation belts during two geomagnetic storms; one representative of a strongly driven magnetosphere (March 31, 2001), and one representative of a more moderate geomagnetic storm (September 24, 1998). In each case, the effect of radial diffusion as a loss process will be examined in the context of initially-trapped particles diffusing through the magnetopause. In contrast, convective radial transport in the tail, providing a source of energetic particles from the plasmasheet to the inner magnetosphere, will be independently examined to determine the potential contribution to radiation belt fluxes via radial transport and trapping of energetic tail particles. Combining the effect of diffusive losses in the inner magnetosphere with the contribution of energetic particles from the tail, weighted by appropriate phase space densities, allows us to comment on the net contribution of radial transport during these two representative events.

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