A Comprehensive Set of Juno In Situ and Remote Sensing Observations of the Ganymede Auroral Footprint

V. Hue, J. R. Szalay, T. K. Greathouse, B. Bonfond, S. Kotsiaros, C. K. Louis, A. H. Sulaiman, G. Clark, F. Allegrini, G. R. Gladstone, C. Paranicas, M. H. Versteeg, A. Mura, A. Moirano, D. J. Gershman, S. J. Bolton, J. E. P. Connerney, M. W. Davis, R. W. Ebert, J.‐C. GérardR. S. Giles, D. C. Grodent, M. Imai, J. A. Kammer, W. S. Kurth, L. Lamy, B. H. Mauk

Research output: Contribution to journalArticlepeer-review

Abstract

Jupiter's satellite auroral footprints are a manifestation of the satellite-magnetosphere interaction of the Galilean moons. Juno's polar elliptical orbit enables crossing the magnetic flux tubes connecting each Galilean moon with their associated auroral emission. Its payload allows measuring the fields and particle population in the flux tubes while remotely sensing their associated auroral emissions. During its thirtieth perijove, Juno crossed the flux tube directly connected to Ganymede's leading footprint spot, a unique event in the entire Juno prime mission. Juno revealed a highly-structured precipitating electron flux, up to 316 mW/m2, while measuring both a small perturbation in the magnetic field azimuthal component and small Poynting flux with an estimated total downward current of 4.2 ± 1.2 kA. Based on the evolution of the footprint morphology and the field and particle measurements, Juno transited for the first time through a region connected to the transhemispheric electron beam of the Ganymede footprint.

Original languageEnglish (US)
Article numbere2021GL096994
JournalGeophysical Research Letters
Volume49
Issue number7
DOIs
StatePublished - Apr 16 2022

Bibliographical note

Funding Information:
This work is dedicated to Franck Hersant, whose generosity, talent and humbleness was an inspirational force. We are grateful to NASA and contributing institutions that have made the Juno mission possible. This work was funded by the NASA New Frontiers Program for Juno (managed by the Jet Propulsion Laboratory) via a subcontract with Southwest Research Institute. This research was supported through Contract 699041X at the University of Iowa, and through Contract NNM06AA75 C with the Southwest Research Institute at Princeton University. BB, JCG, and DG acknowledge funding for this research by a PRODEX contract of ESA, managed with the help of BELSPO. CL's work at DIAS is supported by the Science Foundation Ireland Grant 18/FRL/6199. LL and CL acknowledge the support from CNES and CNRS/INSU programs of planetology and heliophysics. The work of MI was supported by the JSPS KAKENHI Grant Number JP20K22371.

Publisher Copyright:
© 2022. American Geophysical Union. All Rights Reserved.

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