The energy of electron beams near the Io footprint derived from radio-astronomy observations.

Details The energy of electron beams near the Io footprint derived from radio-astronomy observations. The energy of electron beams near the Io footprint derived from radio-astronomy observations.

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm41b1672m&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM41B-1672

Computer Science

Sound

2704 Auroral Phenomena (2407), 2716 Energetic Particles: Precipitating, 2756 Planetary Magnetospheres (5443, 5737, 6033)

Scientific paper

The energy of Jupiter-Io auroral electrons can be inferred through the analysis of decametric radio emissions, especially that of millisecond bursts. Jovian millisecond (or S-)bursts are intense impulsive decametric radio bursts drifting in frequency in tens of milliseconds. Previous analyses suggest that S-bursts are cyclotron-maser emission in the flux tubes connecting Io or Io's wake to Jupiter. Electrons are thought to be accelerated from Io to Jupiter. Near Jupiter, a loss cone appears in the magnetically mirrored electron population, which is able to amplify extraordinary (X) mode radio waves. Most of the theories about their origin include an interpretation of their frequency drift. We have analysed two sets of data collected at the DAM Nançay and Karkhov radio-telescopes; they are consistent with the above scenario. In addition, we confirm that the frequency drift df/dt(f) is negative on average and decreases in absolute value at high frequencies, consistent with the adiabatic theory of particles motion. We find a typical energy of 4 keV for the emitting electrons. In many cases, we find evidence of localized ~ 1 kV electric potential jumps at high latitudes along magnetic field lines connecting Io or Io's wake to Jupiter. These potential jumps are stable over tens of minutes and propagate upward with a velocity of the order of the sound velocity. We will discuss the consistency of such ~ 4 keV electron populations with other energy estimates derived from observations of the UV Jupiter-Io auroras.

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