@article{1433d648f9d84365b37c4e340b3737ed,
title = "In situ observations connected to the io footprint tail aurora",
abstract = " The Juno spacecraft crossed flux tubes connected to the Io footprint tail at low Jovian altitudes on multiple occasions. The transits covered longitudinal separations of approximately 10° to 120° along the footprint tail. Juno{\textquoteright}s suite of magnetospheric instruments acquired detailed measurements of the Io footprint tail. Juno observed planetward electron energy fluxes of ~70 mW/m 2 near the Io footprint and ~10 mW/m 2 farther down the tail, along with correlated, intense electric and magnetic wave signatures, which also decreased down the tail. All observed electron distributions were broad in energy, suggesting a dominantly broadband acceleration process, and did not show any broad inverted-V structure that would be indicative of acceleration by a quasi-static, discrete, parallel potential. Observed waves were primarily below the proton cyclotron frequency, yet identification of a definitive wave mode is elusive. Beyond 40° down the footprint tail, Juno observed depleted upward loss cones, suggesting that the broadband acceleration occurred at distances beyond Juno{\textquoteright}s transit distance of 1.3 to 1.7 R J . For all transits, Juno observed fine structure on scales of approximately tens of kilometers and confirmed independently with electron and wave measurements that a bifurcated tail can intermittently exist.",
author = "Szalay, {J. R.} and B. Bonfond and F. Allegrini and F. Bagenal and S. Bolton and G. Clark and Connerney, {J. E.P.} and Ebert, {R. W.} and Ergun, {R. E.} and Gladstone, {G. R.} and D. Grodent and Hospodarsky, {G. B.} and V. Hue and Kurth, {W. S.} and S. Kotsiaros and Levin, {S. M.} and P. Louarn and B. Mauk and McComas, {D. J.} and J. Saur and Valek, {P. W.} and Wilson, {R. J.}",
note = "Funding Information: The authors would like to thank many Juno team members that made these observations possible. We also thank Rahul Kumar for the insightful discussions on wave-particle interactions and Drake Ranquist for the magnetic field mapping codes. The Juno data used in this study can be obtained from the Planetary Data System (PDS) at http://pds.nasa.gov/. B. B. and D.G. acknowledge financial support from the Belgian Federal Science Policy Office (BELSPO) via the PRODEX Programme of ESA. B.B. is a Research Associate of the Fonds de la Recherche Scientifique-FNRS. The research efforts at the University of Iowa and University of Colorado are supported by NASA through Contracts 699041X and 699050X with the Southwest Research Institute. We thank two anonymous reviewers for their constructive comments. Funding Information: The authors would like to thank many Juno team members that made these observations possible. We also thank Rahul Kumar for the insightful discussions on wave-particle interactions and Drake Ranquist for the magnetic field mapping codes. The Juno data used in this study can be obtained from the Planetary Data System (PDS) at http://pds.nasa.gov/. B. B. and D.G. acknowledge financial support from the Belgian Federal Science Policy Office (BELSPO) via the PRODEX Programme of ESA. B.B. is a Research Associate of the Fonds de la Recherche Scientifique - FNRS. The research efforts at the University of Iowa and University of Colorado are supported by NASA through Contracts 699041X and 699050X with the Southwest Research Institute. We thank two anonymous reviewers for their constructive comments. Publisher Copyright: {\textcopyright}2018. American Geophysical Union. All Rights Reserved.",
year = "2018",
doi = "10.1029/2018JE005752",
language = "English (US)",
volume = "123",
pages = "3061--3077",
journal = "Journal of Geophysical Research E: Planets",
issn = "2169-9097",
number = "11",
}