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Diffuse auroral precipitation in the jovian upper atmosphere and magnetospheric electron flux variability |
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| Authors: | Bidushi Bhattacharya Richard M Thorne Krishan K Khurana |
| Institution: | a Spitzer Science Center, Caltech, MS 220-6, 1200 E. California Blvd., Pasadena, CA 91125, USA b Department of Atmospheric Sciences, UCLA, 7127 MS, Box 951565, 405 Hilgard Ave., Los Angeles, CA 90095, USA c Applied Physics Laboratory, The Johns Hopkins University, 11100 Johns Hopkins Road, Laurel, MD 20723, USA d Institute of Geophysics and Planetary Physics, UCLA, Box 951567, 405 Hilgard Ave., Los Angeles, CA 90095, USA e Department of Physics and Astronomy, The University of Iowa, 203 Van Allen Hall, Iowa City, IA 52242, USA |
| Abstract: | The deposition of energetic electrons in Jupiter's upper atmosphere provides a means, via auroral observations, of monitoring electron and plasma wave activity within the magnetosphere. Not only does particle precipitation indicate a potential change in atmospheric chemistry, it allows for the study of episodic, pronounced flux enhancements in the energetic electron population. A study has been made of the effects of such electron injections into the jovian magnetosphere and of their ability to provide the source population for variations in diffuse auroral emissions. To identify the source region of precipitating auroral electrons, we have investigated the pitch-angle distributions of high-resolution Galileo Energetic Particle Detector (EPD) data that indicate strong flux levels near the loss cone. The equatorial source region of precipitating electrons has been determined from the locations of Galileo's in situ measurements by tracing magnetic field lines using the KK97 model. The primary source region for Jupiter's diffuse aurora appears to lie in the magnetic equator at 15-40 RJ, with the predominant contribution to precipitation flux (tens of ergs cm−2 s−1 sr−1) stemming from <30 RJ. Variability of flux for energetic electrons in this region is also important to the irradiation of surfaces and atmospheres for the Galilean moons: Europa, Ganymede, and Callisto. The average diffuse auroral precipitation flux has been shown to vary by as much as a factor of six at a given radial location. This variability appears to be associated with electron injection events that have been identified in high-resolution Galileo EPD data. These electron flux enhancements are also associated with increased whistler-mode wave activity and magnetic field perturbations, as detected by the Galileo Plasma Wave Subsystem (PWS) and Magnetometer (MAG), respectively. Resonant interactions with the whistler-mode waves cause electron pitch-angle scattering and lead to pitch-angle isotropization and precipitation. |
| Keywords: | Aurorae Jupiter atmosphere Jupiter magnetosphere |
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