Jupiter's Synchrotron Radiation Mapped with the Very Large Array from 1981 to 1998

Details Jupiter's Synchrotron Radiation Mapped with the Very Large Array from 1981 to 1998 Jupiter's Synchrotron Radiation Mapped with the Very Large Array from 1981 to 1998

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apjs..161..520k&link_type=abstract

The Astrophysical Journal Supplement Series, Volume 161, Issue 2, pp. 520-550.

Astronomy and Astrophysics

Astronomy

1

Planets And Satellites: Individual: Jupiter, Radio Continuum: Solar System

Scientific paper

We present Jupiter synchrotron radiation data obtained over a period of 18 yr (1.5 Jovian yr) taken at the VLA at ~20 cm. We look at intensity, polarization, Jovicentric distance, and magnetic latitude and compare the data to a model to distinguish variations over time from variations caused by viewing geometry, i.e., changing DE. No obvious changes in the nature of Jupiter's intrinsic synchrotron radiation were detected other than variations in intensity from year to year. Additionally, a comparison between the data and model at all DE indicate that Jupiter's magnetic field is much more complex than Connerney's O6 magnetic field model we used. Specifically, the intensity and polarization of the main radiation peaks of the model at λCML~275deg-360deg show the largest deviations from the data in the main radiation peaks. Moreover, the radiation peaks in the model Jovian distances are overall farther away than in the data, which is an effect of various parameters such as the radial diffusion coefficient, the generic loss term in the diffusion coefficient, and the energy spectrum of electrons. Despite the differences between the data and model in intensity, polarization, and Jovian distance, the modeled magnetic latitude provides an excellent fit to the data.

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