1) Periodicities Related to Saturn's Magnetospheric Dynamics

2) A Global View of Heating Processes in Jupiter’s
Magnetosphere
3)  Mass and Magnetic Flux Transport in Jupiter’s Magnetodisc: Juno Observations with Global Insight from GAMERA

1) Saturn’s magnetosphere exhibits periodicities ranging from minutes to days. Saturn’s quasi-period 60 minutes (QP60) and ∼10.7 hour planetary period oscillation (PPO) are well documented. However, documentation of periodicities outside of the QP60 and PPO is lacking, as well as an understanding of the interconnectedness of their drivers. We provide a study of Saturn’s magnetospheric periodicities, by analysis of Cassini magnetometer (MAG) and Cassini plasma spectrometer (CAPS) data through various signal processing techniques.

2) The Juno mission,  in conjunction with past missions and Earth-based observations, has provided a wealth of information on Jupiter’s magnetosphere. This magnetosphere is governed by Jupiter’s strong magnetic field, rapid 10-hour rotation, and a large internal plasma source: the volcanic moon Io. Due to the scale of the Jovian magnetosphere, reconnection and magnetic flux circulation are likely completely internally driven processes (i.e., the Vasylunius cycle) with the solar wind providing perturbations; this is unlike the Earth, where the solar wind Bz is the main driver. Juno has observed the magnetosphere across all local times on the night side and has both high-latitude, mid-latitude, and equatorial observations. However, this single thread of data as seen by Juno limits the perspective and available global context for understanding large scale magnetic flux circulation and dynamics in the jovian system. Global numerical models, such as the Grid Agnostic MHD for Extended Research Applications (GAMERA) code can provide both global context and synthetic satellite trajectories to compare to the observations. In this study we present results from a GAMERA simulation highlighting the location, dynamics, and the three-dimensional structure of reconnection and heating events and how they result in the average equatorial temperature radial profile observed by Juno JADE. We also discuss the likelihood of Juno seeing these events, and how they manifest in observations. We achieve this by comparing the observations made by Juno to an ensemble of synthetic Juno trajectories in the simulation. The primary focus is on the magnetic field observations, but also includes comparisons to JADE plasma properties (i.e., flows, density, temperature) where available. The ionospheric signatures of these events are also briefly discussed.

3) Understanding how mass and magnetic flux move through planetary magnetospheres is essential for interpreting their overall dynamics and structure. Jupiter is a rapid rotator and has an internal plasma source. Together, these factors create a dense, equatorially confined magnetodisc where mass and magnetic flux transport play a major role. We present an analysis of mass and magnetic flux transport in this region using Juno MAG, JADE, and JEDI observations along with a global MHD model, GAMERA, which provides critical context beyond the spacecraft’s orbit. Synthetic Juno-like paths are sampled from the simulation and run through the same processing method as the data, allowing for a direct comparison of modeled and observed transport values. We find that these transport quantities vary with both local time and radial distance, revealing structure in how plasma and magnetic flux are redistributed throughout the magnetodisc. To explore how these processes may vary across rapidly rotating systems, we also compare Jupiter’s transport behavior with that observed at Saturn, highlighting both differences and similarities in how mass and magnetic flux are redistributed within their magnetodiscs.