Energetic Electrons in Jupiter's Magnetosphere

Abstract

view Abstract Citations (71) References (58) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Energetic Electrons in Jupiter's Magnetosphere Coroniti, F. V. Abstract A theoretical model for the energetic electron fluxes in the Jovian magnetosphere is developed. Electrons are transported inward from the solar wind or Jovian magnetospheric tail by radial diffusion. The radial diffusion is driven by fluctuating ionospheric dynamo electric fields associated with a neutral- wind tidal eigenmode at ionospheric altitudes. The tidal mode is excited by the electromagnetic coupling of the solar wind to the polar ionosphere; the radial diffusion coefficient which results from disturbed solar-wind flows is 2 X 1 L3 Rj2 per day. Two injection models are considered: (1) electron penetration through the dayside magnetopause-low-energy model; and (2) injection of electrons from an assumed magnetospheric tail high-energy model. Both thermal solar-wind electrons and energetic solar-flare electrons are considered. In the outer zone (7 < L < 20) the electron fluxes are limited to a stably trapped level by whistler-mode precipitation loss. The Galilean satellites are assumed to sweep out all electrons which have access to the satellites. In the inner zone (1.2 < L < 4), a steady-state radial diffusion equation with synchrotron energy loss is solved to the relativistic electron-flux profile, the mean energy, and the total synchrotron power emitted by a flux tube. The synchrotron-emission bandwidth and the flux density at Earth are estimated; the tail-injection model yields the best agreement with the radiometric data. Subject headings: atmospheres, planetary - hydromagnetics - Jupiter - solar wind Publication: The Astrophysical Journal Supplement Series Pub Date: March 1974 DOI: 10.1086/190296 Bibcode: 1974ApJS...27..261C full text sources ADS |