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Jupiter's X-ray and EUV auroras monitored by Chandra, XXM-Newton, and Hisaki satellite

Badman, S. V.; Branduardi-Raymont, G.; Dunn, W. R.; Elsner, R. F.; Ezoe, Y.; Fujimoto, M.; Gladstone, G. R.; Hasegawa, H.; Kimura, T.; Kraft, R. P.; Masters, A.; Murakami, G.; Murray, S. S.; Roediger, E.; Tao, C.; Tsuchiya, F.; Vogt, M. F.; Yamazaki, A.; Yoshikawa, I.; Yoshioka, K.

Authors

S. V. Badman

G. Branduardi-Raymont

W. R. Dunn

R. F. Elsner

Y. Ezoe

M. Fujimoto

G. R. Gladstone

H. Hasegawa

T. Kimura

R. P. Kraft

A. Masters

G. Murakami

S. S. Murray

Dr Elke Roediger E.Roediger@hull.ac.uk
Senior Lecturer/ Director of Studies for Physics

C. Tao

F. Tsuchiya

M. F. Vogt

A. Yamazaki

I. Yoshikawa

K. Yoshioka

Abstract

Jupiter's X-ray auroral emission in the polar cap region results from particles which have undergone strong field-aligned acceleration into the ionosphere. The origin of precipitating ions and electrons and the time variability in the X-ray emission are essential to uncover the driving mechanism for the high-energy acceleration. The magnetospheric location of the source field line where the X-ray is generated is likely affected by the solar wind variability. However, these essential characteristics are still unknown because the long-term monitoring of the X-rays and contemporaneous solar wind variability has not been carried out. In April 2014, the first long-term multiwavelength monitoring of Jupiter's X-ray and EUV auroral emissions was made by the Chandra X-ray Observatory, XMM-Newton, and Hisaki satellite. We find that the X-ray count rates are positively correlated with the solar wind velocity and insignificantly with the dynamic pressure. Based on the magnetic field mapping model, a half of the X-ray auroral region was found to be open to the interplanetary space. The other half of the X-ray auroral source region is magnetically connected with the prenoon to postdusk sector in the outermost region of the magnetosphere, where the Kelvin-Helmholtz (KH) instability, magnetopause reconnection, and quasiperiodic particle injection potentially take place. We speculate that the high-energy auroral acceleration is associated with the KH instability and/or magnetopause reconnection. This association is expected to also occur in many other space plasma environments such as Saturn and other magnetized rotators.

Journal Article Type Article
Publication Date Mar 1, 2016
Journal Journal of geophysical research : space physics
Print ISSN 2169-9402
Electronic ISSN 2169-9402
Publisher American Geophysical Union
Peer Reviewed Peer Reviewed
Volume 121
Issue 3
Pages 2308-2320
Institution Citation Badman, S. V., Branduardi-Raymont, G., Dunn, W. R., Elsner, R. F., Ezoe, Y., Fujimoto, M., …Yoshioka, K. (2016). Jupiter's X-ray and EUV auroras monitored by Chandra, XXM-Newton, and Hisaki satellite. Journal of Geophysical Research: Space Physics, 121(3), 2308-2320. https://doi.org/10.1002/2015ja021893
DOI https://doi.org/10.1002/2015ja021893
Keywords Jupiter, X-ray, Magnetosphere
Publisher URL http://onlinelibrary.wiley.com/doi/10.1002/2015JA021893/abstract;jsessionid=BE031B99A7BC7F5343A61F4B229D752D.f04t04
Copyright Statement ©2016. American Geophysical Union. All Rights Reserved.
Additional Information This is a copy of an article published in: Journal of geophysical research : space physics, 2016, v.121 issue 3.

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Copyright Statement
©2016. American Geophysical Union. All Rights Reserved.



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