In the present work we used unique data on the magnetic field in the Jovian magnetosphere measured by the Juno spacecraft. The data allowed us to determine optimal parameters of the magnetodisc in the paraboloid magnetospheric model and find the ways to qualitatively improve the model.

The reconnection efficiency of the solar-wind-magnetized planet interaction depends on the conditions in the magnetized plasma flow passing the planet. When the reconnection efficiency is very low, the interplanetary magnetic field does not penetrate the magnetosphere. We study this issue for Saturn using Cassini magnetometer data, images of Saturn's aurora obtained by the HST, and the paraboloid model of Saturn's magnetospheric magnetic field. We conclude that the open model is preferable.

The paraboloid model of Saturn’s magnetosphere describes the magnetic field of the planet, the ring current, magnetopause current, and the tail current. The model parameters are determined by comparison with the Cassini magnetic field data from 18 near-equatorial passes that span wide ranges of LT. The best-fit model parameters are employed to determine how the parameters vary with the subsolar distance of the magnetopause, governed by pressure balance at the magnetospheric boundary.