Rights statement: This is the peer reviewed version of the following article: Kimura, T., et al. (2016), Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite, J. Geophys. Res. Space Physics, 121, doi:10.1002/2015JA021893 which has been published in final form at http://onlinelibrary.wiley.com/doi/10.1002/2015JA021893/abstract This article may be used for non-commercial purposes in accordance With Wiley Terms and Conditions for self-archiving.
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Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
}
TY - JOUR
T1 - Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite
AU - Kimura, T.
AU - Kraft, R. P.
AU - Elsner, R. F.
AU - Branduardi-Raymont, Graziella
AU - Gladstone, G. R.
AU - Tao, C.
AU - Yoshioka, Kazuo
AU - Murakami, G.
AU - Yamazaki, A.
AU - Tsuchiya, F.
AU - Vogt, M. F.
AU - Masters, Adam
AU - Hasegawa, H.
AU - Badman, Sarah Victoria
AU - Roediger, E.
AU - Ezoe, Y.
AU - Dunn, W. R.
AU - Yoshikawa, I.
AU - Fujimoto, M.
AU - Murray, S. S.
N1 - This is the peer reviewed version of the following article: Kimura, T., et al. (2016), Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and Hisaki satellite, J. Geophys. Res. Space Physics, 121, doi:10.1002/2015JA021893 which has been published in final form at http://onlinelibrary.wiley.com/doi/10.1002/2015JA021893/abstract This article may be used for non-commercial purposes in accordance With Wiley Terms and Conditions for self-archiving.
PY - 2016/3/22
Y1 - 2016/3/22
N2 - 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.
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.
U2 - 10.1002/2015JA021893
DO - 10.1002/2015JA021893
M3 - Journal article
SP - 2308
EP - 2320
JO - Journal of Geophysical Research: Space Physics
JF - Journal of Geophysical Research: Space Physics
SN - 2169-9402
ER -