Properties of Ion‐Inertial Scale Plasmoids Observed by the Juno Spacecraft in the Jovian Magnetotail.

We expand on previous observations of magnetic reconnection in Jupiter's magnetosphere by constructing a survey of ion‐inertial scale plasmoids in the Jovian magnetotail. We developed an automated detection algorithm to identify reversals in the Bθ ${B}_{\theta }$ component and performed the minimum variance analysis for each identified plasmoid to characterize its helical structure. The magnetic field observations were complemented by data collected using the Juno Waves instrument, which is used to estimate the total electron density, and the JEDI energetic particle detectors. We identified 87 plasmoids with "peak‐to‐peak" durations between 10 and 300 s. Thirty‐one plasmoids possessed a core field and were classified as flux‐ropes. The other 56 plasmoids had minimum field strength at their centers and were termed O‐lines. Out of the 87 plasmoids, 58 had in situ signatures shorter than 60 s, despite the algorithm's upper limit being 300 s, suggesting that smaller plasmoids with shorter durations were more likely to be detected by Juno. We estimate the diameter of these plasmoids assuming a circular cross section and a travel speed equal to the Alfven speed in the surrounding lobes. Using the electron density inferred by Waves, we contend that these plasmoid diameters were within an order of the local ion‐inertial length. Our results demonstrate that magnetic reconnection in the Jovian magnetotail occurs at ion scales like in other space environments. We show that ion‐scale plasmoids would need to be released every 0.1 s or less to match the canonical 1 ton/s rate of plasma production due to Io. Key Points: We identify and analyze 87 ion‐inertial scale plasmoids (56 O‐lines, 31 flux‐ropes) in the Jovian magnetotail using an automated algorithmNorth‐South field reversals with peak‐to‐peak durations less than 60 s are more common than those with durations between 60 and 300 sIon‐inertial scale plasmoids alone cannot account for the >500 kg/s loss‐rate deficit unless they are being produced every ∼0.1 s or less [ABSTRACT FROM AUTHOR]