Spatially Asymmetric Increase in Hot Electron Fraction in the Io Plasma Torus During Volcanically Active Period Revealed by Observations by Hisaki/EXCEED From November 2014 to May 2015

R. Hikida, K. Yoshioka, F. Tsuchiya, M. Kagitani, T. Kimura, F. Bagenal, N. Schneider, G. Murakami, A. Yamazaki, H. Kita, E. Nerney, I. Yoshikawa

研究成果: Article査読

4 被引用数 (Scopus)

抄録

The satellite Io, which has volcanoes and is located at 5.9 RJ from the center of Jupiter, is a powerful plasma source in the magnetosphere. The heavy ions originating from Io form a torus-like structure and emit radiation. The pickup energy and hot electrons are believed to power the Io plasma torus. Voyager data showed that a trace amount of hot electrons (at several hundreds of eV) exist in the torus. The origin of hot electrons, that is, plasma heating and/or transport mechanisms, have been mentioned in previous research. However, the contribution of each mechanism toward supplying hot electrons remains poorly understood. To address this issue, we explored the time variation and spatial structure of hot electrons by spectroscopic observations using the Hisaki satellite. In this study, the radial distributions of plasma densities and temperatures were derived from the emission line intensities in the extreme ultraviolet range of day of year (DOY) 331 in 2014 to DOY 134 in 2015, which includes the Io's volcanically active period. We found that hot electrons inside the torus began to increase particularly on the duskside ~40 days after the onset of volcanic activity. This result suggests that the mass increase in the torus with volcanic activity enhanced the plasma transport from the outside within a specific region or via a local heating process.

本文言語English
論文番号e2019JA027100
ジャーナルJournal of Geophysical Research: Space Physics
125
3
DOI
出版ステータスPublished - 2020 3 1

ASJC Scopus subject areas

  • 宇宙惑星科学
  • 地球物理学

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