Home > Research > Publications & Outputs > Variation of Jupiter's aurora observed by Hisak...

Associated organisational unit

Electronic data

  • Tao_et_al-2015-Jupiter_Hisaki2

    Rights statement: ©2015 American Geophysical Union. All rights reserved

    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

Variation of Jupiter's aurora observed by Hisaki/EXCEED: 2. estimations of auroral parameters and magnetospheric dynamics

Research output: Contribution to journalJournal article

Published
  • Chihiro Tao
  • Tomoki Kimura
  • Sarah V. Badman
  • Nicolas André
  • Fuminori Tsuchiya
  • Go Murakami
  • Kazuo Yoshioka
  • Ichiro Yoshikawa
  • Atsushi Yamazaki
  • Masaki Fujimoto
Close
<mark>Journal publication date</mark>05/2016
<mark>Journal</mark>Journal of Geophysical Research: Space Physics
Issue number5
Volume121
Number of pages17
Pages (from-to)4055-4071
<mark>State</mark>Published
Early online date21/07/15
<mark>Original language</mark>English

Abstract

Jupiter's auroral parameters are estimated from observations by a spectrometer EXCEED (Extreme Ultraviolet Spectroscope for Exospheric Dynamics) onboard JAXA's Earth-orbiting planetary space telescope Hisaki. EXCEED provides continuous auroral spectra covering the wavelength range over 80–148 nm from the whole northern polar region. The auroral electron energy is estimated using a hydrocarbon color ratio adopted for the wavelength range of EXCEED, and the emission power in the long wavelength range 138.5–144.8 nm is used as an indicator of total emitted power before hydrocarbon absorption and auroral electron energy flux. The quasi-continuous observations by Hisaki provide the auroral electron parameters and their relation under different auroral activity levels. Short- (within < one planetary rotation) and long-term (> one planetary rotation) enhancements of auroral power accompany increases of the electron number flux rather than the electron energy variations. The relationships between the auroral electron energy (~70–400 keV) and flux (1026–1027 /s, 0.08–0.9 μA/m2) estimated from the observations over a 40-day interval are in agreement with field-aligned acceleration theory when incorporating probable magnetospheric parameters. Applying the electron acceleration theory to each observation point, we explore the magnetospheric source plasma variation during these power-enhanced events. Possible scenarios to explain the derived variations are (i) an adiabatic variation of the magnetospheric plasma under a magnetospheric compression and/or plasma injection, and (ii) a change of the dominant auroral component from the main emission (main aurora) to the emission at the open-closed boundary.

Bibliographic note

©2015 American Geophysical Union. All rights reserved