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    Rights statement: ©2017. The Authors. This is an open access article under the terms of the Creative Commons Attribution License, which permits use, distribution and reproduction in any medium, provided the original work is properly cited.

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Characterization of Jupiter's secondary auroral oval and its response to hot plasma injections

Research output: Contribution to journalJournal article

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Characterization of Jupiter's secondary auroral oval and its response to hot plasma injections. / Gray, Rebecca; Badman, Sarah Victoria; Woodfield, E. E.; Tao, C.

In: Journal of Geophysical Research: Space Physics, Vol. 122, No. 6, 28.06.2017, p. 6415-6429.

Research output: Contribution to journalJournal article

Harvard

Gray, R, Badman, SV, Woodfield, EE & Tao, C 2017, 'Characterization of Jupiter's secondary auroral oval and its response to hot plasma injections' Journal of Geophysical Research: Space Physics, vol. 122, no. 6, pp. 6415-6429. https://doi.org/10.1002/2017JA024214

APA

Gray, R., Badman, S. V., Woodfield, E. E., & Tao, C. (2017). Characterization of Jupiter's secondary auroral oval and its response to hot plasma injections. Journal of Geophysical Research: Space Physics, 122(6), 6415-6429. https://doi.org/10.1002/2017JA024214

Vancouver

Gray R, Badman SV, Woodfield EE, Tao C. Characterization of Jupiter's secondary auroral oval and its response to hot plasma injections. Journal of Geophysical Research: Space Physics. 2017 Jun 28;122(6):6415-6429. https://doi.org/10.1002/2017JA024214

Author

Gray, Rebecca ; Badman, Sarah Victoria ; Woodfield, E. E. ; Tao, C. / Characterization of Jupiter's secondary auroral oval and its response to hot plasma injections. In: Journal of Geophysical Research: Space Physics. 2017 ; Vol. 122, No. 6. pp. 6415-6429.

Bibtex

@article{37548249056b48ff9385fc5801feee9d,
title = "Characterization of Jupiter's secondary auroral oval and its response to hot plasma injections",
abstract = "We present Jovian auroral observations from the 2014 January Hubble Space Telescope (HST) campaign and characterize the auroral second oval feature with particular attention to the response to hot plasma injections. The location of the second oval feature lies between the Ganymede and Europa moon footprint contours between 150 and 240° system III longitude, corresponding to a source in the inner magnetosphere between 9 and 13 RJ. At the examined longitudes, this is in the same region of 11–16 RJ known as the pitch angle distribution boundary, beyond which electrons are thought to be scattered into a field-aligned configuration and cause auroral precipitation. The feature is enhanced in both brightness and longitudinal spread 1–3 days after large hot plasma injections. The precipitating electrons have a higher-energy and lower flux than the electrons generating large injection signatures. We suggest that wave-particle interactions are responsible for the scattering of electrons in this region. We also suggest that the plasma injections can act as a temperature anisotropy and particle source to enhance electron scattering into the aurora and the brightness of the second oval feature. Changes to the magnetic field topology around an injection may also generate shear Alfv{\'e}n waves and therefore accelerate electrons parallel to the magnetic field resulting in precipitation.",
author = "Rebecca Gray and Badman, {Sarah Victoria} and Woodfield, {E. E.} and C. Tao",
note = "{\circledC}2017. The Authors. This is an open access article under the terms of the Creative Commons Attribution License, which permits use, distribution and reproduction in any medium, provided the original work is properly cited.",
year = "2017",
month = "6",
day = "28",
doi = "10.1002/2017JA024214",
language = "English",
volume = "122",
pages = "6415--6429",
journal = "Journal of Geophysical Research: Space Physics",
issn = "2169-9402",
publisher = "Blackwell Publishing Ltd",
number = "6",

}

RIS

TY - JOUR

T1 - Characterization of Jupiter's secondary auroral oval and its response to hot plasma injections

AU - Gray, Rebecca

AU - Badman, Sarah Victoria

AU - Woodfield, E. E.

AU - Tao, C.

N1 - ©2017. The Authors. This is an open access article under the terms of the Creative Commons Attribution License, which permits use, distribution and reproduction in any medium, provided the original work is properly cited.

PY - 2017/6/28

Y1 - 2017/6/28

N2 - We present Jovian auroral observations from the 2014 January Hubble Space Telescope (HST) campaign and characterize the auroral second oval feature with particular attention to the response to hot plasma injections. The location of the second oval feature lies between the Ganymede and Europa moon footprint contours between 150 and 240° system III longitude, corresponding to a source in the inner magnetosphere between 9 and 13 RJ. At the examined longitudes, this is in the same region of 11–16 RJ known as the pitch angle distribution boundary, beyond which electrons are thought to be scattered into a field-aligned configuration and cause auroral precipitation. The feature is enhanced in both brightness and longitudinal spread 1–3 days after large hot plasma injections. The precipitating electrons have a higher-energy and lower flux than the electrons generating large injection signatures. We suggest that wave-particle interactions are responsible for the scattering of electrons in this region. We also suggest that the plasma injections can act as a temperature anisotropy and particle source to enhance electron scattering into the aurora and the brightness of the second oval feature. Changes to the magnetic field topology around an injection may also generate shear Alfvén waves and therefore accelerate electrons parallel to the magnetic field resulting in precipitation.

AB - We present Jovian auroral observations from the 2014 January Hubble Space Telescope (HST) campaign and characterize the auroral second oval feature with particular attention to the response to hot plasma injections. The location of the second oval feature lies between the Ganymede and Europa moon footprint contours between 150 and 240° system III longitude, corresponding to a source in the inner magnetosphere between 9 and 13 RJ. At the examined longitudes, this is in the same region of 11–16 RJ known as the pitch angle distribution boundary, beyond which electrons are thought to be scattered into a field-aligned configuration and cause auroral precipitation. The feature is enhanced in both brightness and longitudinal spread 1–3 days after large hot plasma injections. The precipitating electrons have a higher-energy and lower flux than the electrons generating large injection signatures. We suggest that wave-particle interactions are responsible for the scattering of electrons in this region. We also suggest that the plasma injections can act as a temperature anisotropy and particle source to enhance electron scattering into the aurora and the brightness of the second oval feature. Changes to the magnetic field topology around an injection may also generate shear Alfvén waves and therefore accelerate electrons parallel to the magnetic field resulting in precipitation.

U2 - 10.1002/2017JA024214

DO - 10.1002/2017JA024214

M3 - Journal article

VL - 122

SP - 6415

EP - 6429

JO - Journal of Geophysical Research: Space Physics

JF - Journal of Geophysical Research: Space Physics

SN - 2169-9402

IS - 6

ER -