Bar Code Events in the Juno-UVS Data: Signature ∼10 MeV Electron Microbursts at Jupiter

B. Bonfond; G. R. Gladstone; D. Grodent; J. C. Gérard; T. K. Greathouse; V. Hue; J. A. Kammer; M. H. Versteeg; M. W. Davis; H. N. Becker; A. Radioti; S. S. Elliott; M. Imai; C. P. Paranicas; S. J. Bolton; S. M. Levin; J. E.P. Connerney

doi:10.1029/2018GL080490

Bar Code Events in the Juno-UVS Data: Signature ∼10 MeV Electron Microbursts at Jupiter

B. Bonfond, G. R. Gladstone, D. Grodent, J. C. Gérard, T. K. Greathouse, V. Hue, J. A. Kammer, M. H. Versteeg, M. W. Davis, H. N. Becker, A. Radioti, S. S. Elliott, M. Imai, C. P. Paranicas, S. J. Bolton, S. M. Levin, J. E.P. Connerney

Research output: Contribution to journal › Article › peer-review

16 Scopus citations

Abstract

One of the most intriguing discoveries of Juno is the quasi-systematic detection of upgoing electrons above the auroral regions. Here we discuss a by-product of the most energetic component of this population: a contamination resembling bar codes in the Juno-UVS images. This pattern is likely caused by bursts of ∼10 MeV electrons penetrating the instrument. These events are mostly detected when Juno's magnetic footprint is located poleward of the main emission relative to the magnetic pole. The signal is not periodic, but the bursts are typically 0.1–1 s apart. They are essentially detected when Juno-UVS is oriented toward Jupiter, indicating that the signal is due to upgoing electrons. The event detections occur between 1 and 7 Jovian radii above the 1-bar level, suggesting that the electron acceleration takes place close to Jupiter and is thus both strong and brief.

Original language	English (US)
Pages (from-to)	12,108-12,115
Journal	Geophysical Research Letters
Volume	45
Issue number	22
DOIs	https://doi.org/10.1029/2018GL080490
State	Published - Nov 28 2018
Externally published	Yes

Bibliographical note

Funding Information:
James W. Alexander, Ingrid J. Daubar, Shawn Kang, and William J. McAlpine are gratefully acknowledged for their work on the Geant4 analysis. B. B. is a Research Associate of the Fonds de la Recherche Scientifique-FNRS. We are grateful to NASA and contributing institutions which have made the Juno mission possible. This work was funded by NASA’s New Frontiers Program for Juno via contract with the Southwest Research Institute. B. B., D. G., A. R., and J.-C. G. acknowledge financial support from the Belgian Federal Science Policy Office (BELSPO) via the PRODEX Programme of ESA. The research at the University of Iowa was supported by NASA through contract 699041X with the Southwest Research Institute. The data included herein are either archived or on schedule to be archived in NASA’s Planetary Data System (http://pds-atmospheres.nmsu.edu/ data_and_services/atmospheres_data/ JUNO/juno.html).

Funding Information:
James W. Alexander, Ingrid J. Daubar, Shawn Kang, and William J. McAlpine are gratefully acknowledged for their work on the Geant4 analysis. B.?B. is a Research Associate of the Fonds de la Recherche Scientifique-FNRS. We are grateful to NASA and contributing institutions which have made the Juno mission possible. This work was funded by NASA's New Frontiers Program for Juno via contract with the Southwest Research Institute. B.?B., D.?G., A.?R., and J.-C.?G. acknowledge financial support from the Belgian Federal Science Policy Office (BELSPO) via the PRODEX Programme of ESA. The research at the University of Iowa was supported by NASA through contract 699041X with the Southwest Research Institute. The data included herein are either archived or on schedule to be archived in NASA's Planetary Data System (http://pds-atmospheres.nmsu.edu/data_and_services/atmospheres_data/JUNO/juno.html).

Publisher Copyright:
©2018. American Geophysical Union. All Rights Reserved.

Keywords

Juno
Juno-UVS
Jupiter
aurora
radiation
relativistic electrons

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10.1029/2018GL080490

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Bonfond, B., Gladstone, G. R., Grodent, D., Gérard, J. C., Greathouse, T. K., Hue, V., Kammer, J. A., Versteeg, M. H., Davis, M. W., Becker, H. N., Radioti, A., Elliott, S. S., Imai, M., Paranicas, C. P., Bolton, S. J., Levin, S. M., & Connerney, J. E. P. (2018). Bar Code Events in the Juno-UVS Data: Signature ∼10 MeV Electron Microbursts at Jupiter. Geophysical Research Letters, 45(22), 12,108-12,115. https://doi.org/10.1029/2018GL080490

Bonfond, B, Gladstone, GR, Grodent, D, Gérard, JC, Greathouse, TK, Hue, V, Kammer, JA, Versteeg, MH, Davis, MW, Becker, HN, Radioti, A, Elliott, SS, Imai, M, Paranicas, CP, Bolton, SJ, Levin, SM & Connerney, JEP 2018, 'Bar Code Events in the Juno-UVS Data: Signature ∼10 MeV Electron Microbursts at Jupiter', Geophysical Research Letters, vol. 45, no. 22, pp. 12,108-12,115. https://doi.org/10.1029/2018GL080490

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title = "Bar Code Events in the Juno-UVS Data: Signature ∼10 MeV Electron Microbursts at Jupiter",

abstract = "One of the most intriguing discoveries of Juno is the quasi-systematic detection of upgoing electrons above the auroral regions. Here we discuss a by-product of the most energetic component of this population: a contamination resembling bar codes in the Juno-UVS images. This pattern is likely caused by bursts of ∼10 MeV electrons penetrating the instrument. These events are mostly detected when Juno's magnetic footprint is located poleward of the main emission relative to the magnetic pole. The signal is not periodic, but the bursts are typically 0.1–1 s apart. They are essentially detected when Juno-UVS is oriented toward Jupiter, indicating that the signal is due to upgoing electrons. The event detections occur between 1 and 7 Jovian radii above the 1-bar level, suggesting that the electron acceleration takes place close to Jupiter and is thus both strong and brief.",

keywords = "Juno, Juno-UVS, Jupiter, aurora, radiation, relativistic electrons",

author = "B. Bonfond and Gladstone, {G. R.} and D. Grodent and G{\'e}rard, {J. C.} and Greathouse, {T. K.} and V. Hue and Kammer, {J. A.} and Versteeg, {M. H.} and Davis, {M. W.} and Becker, {H. N.} and A. Radioti and Elliott, {S. S.} and M. Imai and Paranicas, {C. P.} and Bolton, {S. J.} and Levin, {S. M.} and Connerney, {J. E.P.}",

note = "Funding Information: James W. Alexander, Ingrid J. Daubar, Shawn Kang, and William J. McAlpine are gratefully acknowledged for their work on the Geant4 analysis. B. B. is a Research Associate of the Fonds de la Recherche Scientifique-FNRS. We are grateful to NASA and contributing institutions which have made the Juno mission possible. This work was funded by NASA{\textquoteright}s New Frontiers Program for Juno via contract with the Southwest Research Institute. B. B., D. G., A. R., and J.-C. G. acknowledge financial support from the Belgian Federal Science Policy Office (BELSPO) via the PRODEX Programme of ESA. The research at the University of Iowa was supported by NASA through contract 699041X with the Southwest Research Institute. The data included herein are either archived or on schedule to be archived in NASA{\textquoteright}s Planetary Data System (http://pds-atmospheres.nmsu.edu/ data_and_services/atmospheres_data/ JUNO/juno.html). Funding Information: James W. Alexander, Ingrid J. Daubar, Shawn Kang, and William J. McAlpine are gratefully acknowledged for their work on the Geant4 analysis. B.?B. is a Research Associate of the Fonds de la Recherche Scientifique-FNRS. We are grateful to NASA and contributing institutions which have made the Juno mission possible. This work was funded by NASA's New Frontiers Program for Juno via contract with the Southwest Research Institute. B.?B., D.?G., A.?R., and J.-C.?G. acknowledge financial support from the Belgian Federal Science Policy Office (BELSPO) via the PRODEX Programme of ESA. The research at the University of Iowa was supported by NASA through contract 699041X with the Southwest Research Institute. The data included herein are either archived or on schedule to be archived in NASA's Planetary Data System (http://pds-atmospheres.nmsu.edu/data_and_services/atmospheres_data/JUNO/juno.html). Publisher Copyright: {\textcopyright}2018. American Geophysical Union. All Rights Reserved.",

year = "2018",

month = nov,

day = "28",

doi = "10.1029/2018GL080490",

language = "English (US)",

volume = "45",

pages = "12,108--12,115",

journal = "Geophysical Research Letters",

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T1 - Bar Code Events in the Juno-UVS Data

T2 - Signature ∼10 MeV Electron Microbursts at Jupiter

AU - Bonfond, B.

AU - Gladstone, G. R.

AU - Grodent, D.

AU - Gérard, J. C.

AU - Greathouse, T. K.

AU - Hue, V.

AU - Kammer, J. A.

AU - Versteeg, M. H.

AU - Davis, M. W.

AU - Becker, H. N.

AU - Radioti, A.

AU - Elliott, S. S.

AU - Imai, M.

AU - Paranicas, C. P.

AU - Bolton, S. J.

AU - Levin, S. M.

AU - Connerney, J. E.P.

N1 - Funding Information: James W. Alexander, Ingrid J. Daubar, Shawn Kang, and William J. McAlpine are gratefully acknowledged for their work on the Geant4 analysis. B. B. is a Research Associate of the Fonds de la Recherche Scientifique-FNRS. We are grateful to NASA and contributing institutions which have made the Juno mission possible. This work was funded by NASA’s New Frontiers Program for Juno via contract with the Southwest Research Institute. B. B., D. G., A. R., and J.-C. G. acknowledge financial support from the Belgian Federal Science Policy Office (BELSPO) via the PRODEX Programme of ESA. The research at the University of Iowa was supported by NASA through contract 699041X with the Southwest Research Institute. The data included herein are either archived or on schedule to be archived in NASA’s Planetary Data System (http://pds-atmospheres.nmsu.edu/ data_and_services/atmospheres_data/ JUNO/juno.html). Funding Information: James W. Alexander, Ingrid J. Daubar, Shawn Kang, and William J. McAlpine are gratefully acknowledged for their work on the Geant4 analysis. B.?B. is a Research Associate of the Fonds de la Recherche Scientifique-FNRS. We are grateful to NASA and contributing institutions which have made the Juno mission possible. This work was funded by NASA's New Frontiers Program for Juno via contract with the Southwest Research Institute. B.?B., D.?G., A.?R., and J.-C.?G. acknowledge financial support from the Belgian Federal Science Policy Office (BELSPO) via the PRODEX Programme of ESA. The research at the University of Iowa was supported by NASA through contract 699041X with the Southwest Research Institute. The data included herein are either archived or on schedule to be archived in NASA's Planetary Data System (http://pds-atmospheres.nmsu.edu/data_and_services/atmospheres_data/JUNO/juno.html). Publisher Copyright: ©2018. American Geophysical Union. All Rights Reserved.

PY - 2018/11/28

Y1 - 2018/11/28

N2 - One of the most intriguing discoveries of Juno is the quasi-systematic detection of upgoing electrons above the auroral regions. Here we discuss a by-product of the most energetic component of this population: a contamination resembling bar codes in the Juno-UVS images. This pattern is likely caused by bursts of ∼10 MeV electrons penetrating the instrument. These events are mostly detected when Juno's magnetic footprint is located poleward of the main emission relative to the magnetic pole. The signal is not periodic, but the bursts are typically 0.1–1 s apart. They are essentially detected when Juno-UVS is oriented toward Jupiter, indicating that the signal is due to upgoing electrons. The event detections occur between 1 and 7 Jovian radii above the 1-bar level, suggesting that the electron acceleration takes place close to Jupiter and is thus both strong and brief.

AB - One of the most intriguing discoveries of Juno is the quasi-systematic detection of upgoing electrons above the auroral regions. Here we discuss a by-product of the most energetic component of this population: a contamination resembling bar codes in the Juno-UVS images. This pattern is likely caused by bursts of ∼10 MeV electrons penetrating the instrument. These events are mostly detected when Juno's magnetic footprint is located poleward of the main emission relative to the magnetic pole. The signal is not periodic, but the bursts are typically 0.1–1 s apart. They are essentially detected when Juno-UVS is oriented toward Jupiter, indicating that the signal is due to upgoing electrons. The event detections occur between 1 and 7 Jovian radii above the 1-bar level, suggesting that the electron acceleration takes place close to Jupiter and is thus both strong and brief.

KW - Juno

KW - Juno-UVS

KW - Jupiter

KW - aurora

KW - radiation

KW - relativistic electrons

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