Rights statement: An edited version of this paper was published by AGU. Copyright 2017 American Geophysical Union. Bonfond, B., J. Saur, D. Grodent, S. V. Badman, D. Bisikalo, V. Shematovich, J.‐C. Gérard, and A. Radioti (2017), The tails of the satellite auroral footprints at Jupiter, J. Geophys. Res. Space Physics, 122, 7985–7996, doi:10.1002/2017JA024370.
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Rights statement: ©2017. American Geophysical Union. All Rights Reserved.
Final published version, 4.81 MB, PDF document
Final published version
Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
}
TY - JOUR
T1 - The tails of the satellite auroral footprints at Jupiter
AU - Bonfond, B.
AU - Saur, J.
AU - Grodent, D.
AU - Badman, S. V.
AU - Bisikalo, D.
AU - Shematovich, V.
AU - Gerard, J. -C.
AU - Radioti, A.
N1 - An edited version of this paper was published by AGU. Copyright 2017 American Geophysical Union. Bonfond, B., J. Saur, D. Grodent, S. V. Badman, D. Bisikalo, V. Shematovich, J.‐C. Gérard, and A. Radioti (2017), The tails of the satellite auroral footprints at Jupiter, J. Geophys. Res. Space Physics, 122, 7985–7996, doi:10.1002/2017JA024370.
PY - 2017/8
Y1 - 2017/8
N2 - The electromagnetic interaction between Io, Europa, and Ganymede and the rotating plasma that surrounds Jupiter has a signature in the aurora of the planet. This signature, called the satellite footprint, takes the form of a series of spots located slightly downstream of the feet of the field lines passing through the moon under consideration. In the case of Io, these spots are also followed by an extended tail in the downstream direction relative to the plasma flow encountering the moon. A few examples of a tail for the Europa footprint have also been reported in the northern hemisphere. Here we present a simplified Alfvenic model for footprint tails and simulations of vertical brightness profiles for various electron distributions, which favor such a model over quasi-static models. We also report here additional cases of Europa footprint tails, in both hemispheres, even though such detections are rare and difficult. Furthermore, we show that the Ganymede footprint can also be followed by a similar tail. Finally, we present a case of a 320 degrees long Io footprint tail, while other cases in similar configurations do not display such a length.
AB - The electromagnetic interaction between Io, Europa, and Ganymede and the rotating plasma that surrounds Jupiter has a signature in the aurora of the planet. This signature, called the satellite footprint, takes the form of a series of spots located slightly downstream of the feet of the field lines passing through the moon under consideration. In the case of Io, these spots are also followed by an extended tail in the downstream direction relative to the plasma flow encountering the moon. A few examples of a tail for the Europa footprint have also been reported in the northern hemisphere. Here we present a simplified Alfvenic model for footprint tails and simulations of vertical brightness profiles for various electron distributions, which favor such a model over quasi-static models. We also report here additional cases of Europa footprint tails, in both hemispheres, even though such detections are rare and difficult. Furthermore, we show that the Ganymede footprint can also be followed by a similar tail. Finally, we present a case of a 320 degrees long Io footprint tail, while other cases in similar configurations do not display such a length.
KW - Jupiter
KW - aurora
KW - Io
KW - Europa
KW - Ganymede
KW - satellite footprint
KW - IO
KW - GANYMEDE
KW - EUROPA
KW - MODEL
KW - ATMOSPHERE
KW - ELECTRONS
KW - CALLISTO
KW - SPOTS
KW - WAKE
U2 - 10.1002/2017JA024370
DO - 10.1002/2017JA024370
M3 - Journal article
VL - 122
SP - 7985
EP - 7996
JO - Journal of Geophysical Research: Space Physics
JF - Journal of Geophysical Research: Space Physics
SN - 2169-9380
IS - 8
ER -