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Characteristics of Jupiter’s X-ray auroral hot spot emissions using Chandra

Characteristics of Jupiter’s X-ray auroral hot spot emissions using Chandra
Characteristics of Jupiter’s X-ray auroral hot spot emissions using Chandra
To help understand and determine the driver of jovian auroral X-rays, we present the first statistical study to focus on the morphology and dynamics of the jovian northern hot spot (NHS) using Chandra data. The catalogue we explore dates from 18 December 2000 up to and including 8 September 2019. Using a numerical criterion, we characterize the typical and extreme behaviour of the concentrated NHS emissions across the catalogue. The mean power of the NHS is found to be 1.91 GW with a maximum brightness of 2.02 Rayleighs (R), representing by far the brightest parts of the jovian X-ray spectrum. We report a statistically significant region of emissions at the NHS center which is always present, the averaged hot spot nucleus (AHSNuc), with mean power of 0.57 GW and inferred average brightness of ∼ 1.2 R. We use a flux equivalence mapping model to link this distinct region of X-ray output to a likely source location and find that the majority of mappable NHS photons emanate from the pre-dusk to pre-midnight sector, coincident with the dusk flank boundary. A smaller cluster maps to the noon magnetopause boundary, dominated by the AHSNuc, suggesting that there may be multiple drivers of X-ray emissions. On application of timing analysis techniques (Rayleigh, Monte Carlo, Jackknife), we identify several instances of statistically significant quasi-periodic oscillations (QPOs) in the NHS photons ranging from ∼ 2.3-min to 36.4-min, suggesting possible links with ultra-low frequency activity on the magnetopause boundary (e.g. dayside reconnection, Kelvin-Helmholtz instabilities).
2169-9380
Weigt, Dale, Michael
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Jackman, C. M.
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Vogt, M.F.
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Manners, H.
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Dunn, William R.
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Gladstone, G.R.
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Kraft, R.P.
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Branduardi-Raymont, Graziella
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Louis, C. K.
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McEntee, S. C.
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Weigt, Dale, Michael
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Jackman, C. M.
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Vogt, M.F.
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Manners, H.
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Dunn, William R.
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Gladstone, G.R.
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Kraft, R.P.
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Branduardi-Raymont, Graziella
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Louis, C. K.
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McEntee, S. C.
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Weigt, Dale, Michael, Jackman, C. M., Vogt, M.F., Manners, H., Dunn, William R., Gladstone, G.R., Kraft, R.P., Branduardi-Raymont, Graziella, Louis, C. K. and McEntee, S. C. (2021) Characteristics of Jupiter’s X-ray auroral hot spot emissions using Chandra. Journal of Geophysical Research: Space Physics, [e2021JA029243]. (doi:10.1029/2021JA029243).

Record type: Article

Abstract

To help understand and determine the driver of jovian auroral X-rays, we present the first statistical study to focus on the morphology and dynamics of the jovian northern hot spot (NHS) using Chandra data. The catalogue we explore dates from 18 December 2000 up to and including 8 September 2019. Using a numerical criterion, we characterize the typical and extreme behaviour of the concentrated NHS emissions across the catalogue. The mean power of the NHS is found to be 1.91 GW with a maximum brightness of 2.02 Rayleighs (R), representing by far the brightest parts of the jovian X-ray spectrum. We report a statistically significant region of emissions at the NHS center which is always present, the averaged hot spot nucleus (AHSNuc), with mean power of 0.57 GW and inferred average brightness of ∼ 1.2 R. We use a flux equivalence mapping model to link this distinct region of X-ray output to a likely source location and find that the majority of mappable NHS photons emanate from the pre-dusk to pre-midnight sector, coincident with the dusk flank boundary. A smaller cluster maps to the noon magnetopause boundary, dominated by the AHSNuc, suggesting that there may be multiple drivers of X-ray emissions. On application of timing analysis techniques (Rayleigh, Monte Carlo, Jackknife), we identify several instances of statistically significant quasi-periodic oscillations (QPOs) in the NHS photons ranging from ∼ 2.3-min to 36.4-min, suggesting possible links with ultra-low frequency activity on the magnetopause boundary (e.g. dayside reconnection, Kelvin-Helmholtz instabilities).

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Accepted/In Press date: 15 August 2021
Published date: 25 August 2021

Identifiers

Local EPrints ID: 451248
URI: http://eprints.soton.ac.uk/id/eprint/451248
ISSN: 2169-9380
PURE UUID: adb223e7-8657-4c84-adae-0b5cccb8e95c

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Date deposited: 14 Sep 2021 21:00
Last modified: 14 Sep 2021 21:00

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Contributors

Author: Dale, Michael Weigt
Author: C. M. Jackman
Author: M.F. Vogt
Author: H. Manners
Author: William R. Dunn
Author: G.R. Gladstone
Author: R.P. Kraft
Author: Graziella Branduardi-Raymont
Author: C. K. Louis
Author: S. C. McEntee

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