Radial diffusion models of energetic electrons and Jupiter's synchrotron radiation. 2: Time variability

Details Radial diffusion models of energetic electrons and Jupiter's synchrotron radiation. 2: Time variability Radial diffusion models of energetic electrons and Jupiter's synchrotron radiation. 2: Time variability

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994jgr....99.2271d&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 99, no. A2, p. 2271-2287

Physics

32

Electron Density (Concentration), Electron Diffusion, Jupiter Atmosphere, Planetary Magnetospheres, Radial Distribution, Radio Emission, Synchrotron Radiation, Atmospheric Turbulence, Electric Fields, Energy Spectra, Magnetic Fields, Mathematical Models, Solar Wind, Time Dependence, Jupiter, Diffusion, Model, Electrons, Radiation, Magnetosphere, Flux, Radiowaves, Emissions, Phase, Amplitude, Density, Decimeter Waves, Parameters, Intensity, Timescale, Calculations, Comparison, Simulation, Boundaries, Solar W

Scientific paper

We used a radial diffusion code for energetic electrons in Jupiter's magnetosphere to investigate variations in Jupiter's radio emission due to changes in the electron phase space density at L shells between 6 and 50, and due to changes in the radial diffusion parameters. We suggest that the observed variations in Jupiter's radio emission are likely caused by changes in the electron phase space density at some boundary L1 is greater than 6, if the primary mode of transport of energetic electrons is radial diffusion driven by fluctuating electric and/or magnetic fields induced by upper atmospheric turbulence. We noticed an excellent empirical correlation, both in phase and relative amplitude, between changes in the solar wind ram pressure and Jupiter's synchrotron radiation if the electron phase space density at the boundary L1 (L1 is approximately equal to 20-50) varies linearly with the square root of the solar wind ram pressure, f is approximately (Nsnu2s)1/2. The calculations were carried out with a diffusion coefficient DLL = DnLn with n = 3. The diffusion coefficient which best fit the observed variations in Jupiter's synchrotron radiation D3 = 1.3 +/- 0.2 x 10-9/s is approximately 0.041/yr, which corresponds to a lagtime of approximately 2 years. We further show that the observed short term (days-weeks) variations in Jupiter's radio emission cannot be explained adequately when radial diffusion is taken into account.

Affiliated with

Also associated with

No associations

Rating

Radial diffusion models of energetic electrons and Jupiter's synchrotron radiation. 2: Time variability does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Radial diffusion models of energetic electrons and Jupiter's synchrotron radiation. 2: Time variability, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Radial diffusion models of energetic electrons and Jupiter's synchrotron radiation. 2: Time variability will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1017063