The awesome thing about space physics is that from just three lines you can determine the state and dynamics of a distant planet’s magnetosphere. Just look at this figure showing Revolution A of the Cassini spacecraft from October 2004.
Here we can actually see that Cassini first flies through a very turbulent region (A), which is the current sheet of the magnetosphere crossing over Cassini multiple times (sign changes in B_phi). Then it gets a little quiter (B) as Cassini remains above the magnetic equator. Closer to the planet we then observe fluxtube interchanges (C), where dense plasma that is frozen-in with the magnetic field lines is thrown outside.
How cool is that? If you’re really interested, you can read
von Papen, M., Saur, J., & Alexandrova, O. (2014). Turbulent magnetic field fluctuations in Saturn’s magnetosphere. Journal of Geophysical Research: Space Physics, 119(4), 2797–2818. https://doi.org/10.1002/2013JA019542