Programme by Session

In the magnetosphere of Saturn, the dominant magnetic field contributors are the internal field and the magnetodisc current sheet. The co-rotating plasma, sourced from the moon Enceladus, that carries the azimuthal current in this equatorial sheet stretches the magnetic field into the characteristic magnetodisc geometry. This current sheet is observed at all local times but has a highly dynamic configuration due to multiple factors, including planetary period oscillations, variable solar wind conditions and the obliquity of Saturn.

In this study, we use the complete magnetic field dataset collected by the Cassini spacecraft to determine the north-south thickness of the magnetodisc current sheet. We identify crossings of the current sheet where a clear signature in the radial field component allows us to constrain the boundaries of the current layer. We begin by investigating the factors that are controlling the variability of the thickness. We then determine how the thickness varies both spatially and temporally with respect to these dynamical processes that are continuously perturbing the current sheet. Finally, we calculate the average thickness as a function of these parameters. Our results are essential for understanding the global configuration of the Saturnian system and how it is modified by the magnetodisc current sheet. They also enable us to better model the most significant current system in the Saturnian magnetosphere.