Further observational support for the lossy radial diffusion model of the inner Jovian magnetosphere

A mathematical model describing radial diffusion, with violation of the third adiabatic invariant and with local losses, is applied to the Pioneer 10 and 11 observations of omnidirectional integral intensities of electrons with energy exceeding 21 MeV. Local losses outside L = 3 are much stronger than synchrotron losses but weaker than the losses one would expect for strong pitch angle diffusion. If radial diffusion is driven by ionospheric winds, as was suggested by Brice and McDonough (1973), it is found that the theoretical solution which best fits the data requires that the radial diffusion coefficient equals 3 x 10 to the -9th L-cubed/s and the lifetime against local losses is approximately a few million seconds.

[1]  D. Sentman,et al.  Whistler mode noise in Jupiter's inner magnetosphere , 1978 .

[2]  J. A. V. Allen,et al.  On determining magnetospheric diffusion coefficients from the observed effects of Jupiter's satellite Io , 1977 .

[3]  J. A. V. Allen,et al.  A determination of the L dependence of the radial diffusion coefficient for protons in Jupiter's inner magnetosphere , 1977 .

[4]  D. Baker,et al.  Radial diffusion in Jupiter's magnetosphere , 1976 .

[5]  F. Scarf,et al.  Some comments on the whistler mode instability at Jupiter , 1976 .

[6]  F. Coroniti,et al.  Lossy radial diffusion of relativistic Jovian electrons. [calculation of synchrotron radiation and electron radiation for Jupiter , 1976 .

[7]  D. Baker,et al.  Energetic electrons in the Jovian magnetosphere , 1976 .

[8]  F. Coroniti.  Dénouement of Jovian radiation belt theory , 1975 .

[9]  D. Baker,et al.  Revised Pioneer 10 absolute electron intensities in the inner Jovian magnetosphere. Progress report , 1975 .

[10]  D N Baker,et al.  Pioneer 11 Observations of Energetic Particles in the Jovian Magnetosphere , 1975, Science.

[11]  D. Baker,et al.  The magnetosphere of Jupiter as observed with Pioneer 10: 1. Instrument and principal findings , 1974 .

[12]  C. Kennel,et al.  Is Jupiter's magnetosphere like a pulsar's or Earth's? , 1974 .

[13]  Thomas R. McDonough,et al.  Jupiter's radiation belts , 1973 .

[14]  C. Kennel,et al.  Jupiter's Magnetosphere , 1977 .

[15]  C. Mcilwain,et al.  Evidence that pitch angle scattering is an important loss mechanism for energetic electrons in the inner radiation belt of Jupiter , 1976 .

[16]  A. Mogro-Campero.  Absorption of radiation belt particles by the inner satellites of Jupiter , 1976 .

[17]  R. Thorne.  The Structure and Stability of Radiation Belt Electrons as Controlled by Wave-Particle Interactions , 1976 .

[18]  T. Northrop,et al.  The electron diffusion coefficient in Jupiter's magnetosphere , 1974 .

[19]  T. Northrop,et al.  The electron diffusion coeffcient in Jupiter's magnetosphere , 1974 .

[20]  N. Herlofson,et al.  Particle Diffusion in the Radiation Belts , 1962 .