Figure 2.

Perturbation plot for Periapsis Pass 16 illustrating a comparison of the observed vector magnetic field (after removal of the internal field using the JRM09 model) and the modeled (r < 30 R _j) magnetodisc field, using the model fit parameters listed in Table 1. From top to bottom we plot the azimuthal, theta, and radial components of the observed (black) and modeled (blue) field. The shaded region represents a strong field region (>1,600 nT) dominated by the planetary field and excluded from consideration. Periapais 16 is an example of a pass fitting the azimuthal component poorly inbound to periJove, while fitting the theta and radial components well. The outbound portion of the periapsis pass has a distinctly different character as a result of an outbound trajectory at higher magnetic latitudes, remaining well above the current‐carrying region.