On asymmetries of turbulent magnetic fluctuations in Jupiter's and Saturn's magnetospheres

Abstract:

Net plasma transport in magnetodiscs around giant planets is outward. Observations of temperature of plasma have showed that expanding plasma is heating up non-adiabatically during this process. Turbulence has been suggested as a source of heating. However, the mechanism and configuration of turbulence in giant magnetospheres are poorly understood. In this study we attempt to build a physical picture of turbulent heating processes in Saturn and Jovian magnetospheres. We use Cassini and Galileo magnetometer data to observe fluctuations of the magnetic field. Power spectra based on weak or strong magnetohydrodynamic (MHD), or kinetic Alfven wave (KAW) turbulence are then used to study turbulent heating. Data sets from different orbits around planets are used to study global turbulent environment of magnetospheres. Here we present findings of asymmetrical configuration of turbulent heating mechanisms of plasma around Jupiter and Saturn.