Home > Research > Publications & Outputs > Jupiter's X-ray and EUV auroras monitored by Ch...

Associated organisational unit

Electronic data

  • xhisaki_kimura_revisedJan16

    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.

    Accepted author manuscript, 1 MB, PDF-document

    Available under license: CC BY-NC: Creative Commons Attribution-NonCommercial 4.0 International License

Links

Text available via DOI:

View graph of relations

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

Research output: Contribution to journalJournal article

Published
  • T. Kimura
  • R. P. Kraft
  • R. F. Elsner
  • Graziella Branduardi-Raymont
  • G. R. Gladstone
  • C. Tao
  • Kazuo Yoshioka
  • G. Murakami
  • A. Yamazaki
  • F. Tsuchiya
  • M. F. Vogt
  • Adam Masters
  • H. Hasegawa
  • Sarah Victoria Badman
  • E. Roediger
  • Y. Ezoe
  • W. R. Dunn
  • I. Yoshikawa
  • M. Fujimoto
  • S. S. Murray
Close
<mark>Journal publication date</mark>22/03/2016
<mark>Journal</mark>Journal of Geophysical Research: Space Physics
Number of pages13
Pages (from-to)2308-2320
<mark>State</mark>Published
Early online date3/02/16
<mark>Original language</mark>English

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.

Bibliographic note

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.