Developments in Jovian radio emissions tomography and observations techniques

Jupiter radio emission is known to be the most powerful nonthermal planetar y radiation. In recent years specifically space-based observations allow us to permanently cover a large frequency band (from 100 kHz up to 40 MHz com bined with ground-based telescopes) of the Jovian spectrum. The Plasma and Wave Science experiment onboard Galileo enables the observation of Jovian k ilometric and hectometric emissions; Wind/WAVES and ground-based telescopes (mainly Decametric Array in Nancay, France, and UTR-2 in Kharkov, Ukraine) cover also hectometric and mainly decametric emissions. Specific geometric al configurations between Cassini approaching Jupiter and Wind spacecraft o rbiting Earth, with Galileo orbiting Jupiter and Wind, in combination with ground-based observations provide a new approach to perform Jovian radio to mography. The tomography technique is used to analyze ray paths of Jovian r adio emission observed in different directions (e.g. solar and anti-solar d irection) and for different declination of Earth. The developments of Jovia n radio emission tomography in recent years treated refraction effects and its connection to the local magnetic field in the radio source as well as t he radio wave propagation through the Io torus and the terrestrial ionosphe re. Most recently ground-based multi-site and simultaneous Jupiter decametr ic radio observations by means of digital spectropolarimeter and waveform r eceiver provide the basis of a new data analysis treatment. The above addre ssed topics are without exemption deeply connected to the plasma structures the radio waves are generated in and propagating through.