Imperial College London
Alternate

DrAdamMasters

Faculty of Natural Sciences, Department of Physics

Senior Lecturer
 
 
 
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a.masters

 
 
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Location

 

6M69Huxley BuildingSouth Kensington Campus

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Summary

 

Publications

Citation

BibTex format

@article{Kimura:2016:10.1002/2015JA021893,
author = {Kimura, T and Kraft, RP and Elsner, RF and Branduardi-Raymont, G and Gladstone, GR and Tao, C and Yoshioka, K and Murakami, G and Yamazaki, A and Tsuchiya, F and Vogt, MF and Masters, A and Hasegawa, H and Badman, SV and Roediger, E and Ezoe, Y and Dunn, WR and Yoshikawa, I and Fujimoto, M and Murray, SS},
doi = {10.1002/2015JA021893},
journal = {Journal of Geophysical Research: Space Physics},
pages = {2308--2320},
title = {Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite},
url = {http://dx.doi.org/10.1002/2015JA021893},
volume = {121},
year = {2016}
}
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RIS format (EndNote, RefMan)

TY  - JOUR
AB  - 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.
AU  - Kimura,T
AU  - Kraft,RP
AU  - Elsner,RF
AU  - Branduardi-Raymont,G
AU  - Gladstone,GR
AU  - Tao,C
AU  - Yoshioka,K
AU  - Murakami,G
AU  - Yamazaki,A
AU  - Tsuchiya,F
AU  - Vogt,MF
AU  - Masters,A
AU  - Hasegawa,H
AU  - Badman,SV
AU  - Roediger,E
AU  - Ezoe,Y
AU  - Dunn,WR
AU  - Yoshikawa,I
AU  - Fujimoto,M
AU  - Murray,SS
DO  - 10.1002/2015JA021893
EP  - 2320
PY  - 2016///
SN  - 2169-9402
SP  - 2308
TI  - Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite
T2  - Journal of Geophysical Research: Space Physics
UR  - http://dx.doi.org/10.1002/2015JA021893
UR  - http://hdl.handle.net/10044/1/33301
VL  - 121
ER  -
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