Characteristics Of Short-Term Variation Of The Jovian Synchrotron Radiation At A Frequency Of 327MHz

Details Characteristics Of Short-Term Variation Of The Jovian Synchrotron Radiation At A Frequency Of 327MHz Characteristics Of Short-Term Variation Of The Jovian Synchrotron Radiation At A Frequency Of 327MHz

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm23a0304n&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM23A-0304

Physics

2720 Energetic Particles: Trapped, 2731 Magnetosphere: Outer, 6220 Jupiter, 6939 Magnetospheric Physics (2700), 6969 Remote Sensing

Scientific paper

The Jovian synchrotron radiation (JSR) is a radio wave emitted from the relativistic electrons in the Jovian radiation belt, which have information of dynamics of high-energy particles and electromagnetic disturbances in the Jovian inner magnetosphere. The intensity variation of JSR, however, has been little understood in its timescales and origin. We have observed JSR for several months a year since 1994 to reveal characteristics of the flux variations especially at the time scales of days to months (short-term) and years (long-term). The regular observations have been made at a frequency of 327MHz by using parabolic cylinder antennas of the Solar Terrestrial Environment Laboratory, Nagoya University, Japan. The observed JSR flux includes apparent variation due to inevitable system gain variation of the radio receiving system. In order to compensate the system gain variation, we have evaluated system gain using a calibration star that was observed quasi-simultaneously with JSR, and made observations of 'actual' galactic back-ground (BG) radiation with the highly stable radio receiving system of Tohoku University. We have also derived the JSR flux densities to improve reliability of the JSR flux densities by revaluation of BG radiation using an other technique to estimate BG: we have observed calibration star which was actually used in the past JSR observations and BG radiation at a time by the electrically beam-switching method, which is just the same observation method as the actual observations for the calibration star and Jupiter. We confirmed JSR fluxes varies by more than 100% during only several days on the solar minimum phase (1995-1996). Though Miyoshi et al., (1999) indicated from the JSR observation at 2.3GHz that a short JSR flux variation is related to intensification of solar UV/EUV as a causality, this result suggests that the occurrence of rapidly enhanced radial diffusion induced by UV/EUV heating in Jupiter's upper atmosphere is not the only plausible mechanism for the JSR at 327MHz. In our presentation, we will introduce characteristics of variations of JSR for 1995-1996 and discuss expected transport processes of high-energy particles in the Jovian radiation belt.

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