Hot electron component in the Io plasma torus confirmed through EUV spectral analysis

DOI PDF Web Site 被引用文献12件 参考文献36件 オープンアクセス
  • K. Yoshioka
    Department of Physics; Rikkyo University; Tokyo Japan
  • I. Yoshikawa
    Department of Earth and Planetary Science; University of Tokyo; Tokyo Japan
  • F. Tsuchiya
    Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
  • M. Kagitani
    Planetary Plasma and Atmospheric Research Center; Tohoku University; Sendai Japan
  • G. Murakami
    Department of Earth and Planetary Science; University of Tokyo; Tokyo Japan

書誌事項

タイトル別名
  • HOT ELECTRONS IN THE IO PLASMA TORUS
公開日
2011-09
資源種別
journal article
権利情報
  • http://doi.wiley.com/10.1002/tdm_license_1
DOI
  • 10.1029/2011ja016583
公開者
American Geophysical Union (AGU)

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説明

[1] The Io plasma torus is composed mainly of sulfur and oxygen ions and their compounds, together with a background of electrons. In addition to those basic components, several in situ observations have shown that a small percentage of the electrons there have been excited to be as much as 100 times hotter than the background electrons. They have a significant impact on the energy balance in the Jovian inner magnetosphere. However, their generation process has not yet been clarified. One difficulty is that the available data about the hot electrons all come from in situ observations which cannot explore the temporal and spatial distributions explicitly. Therefore, remote sensing which can take a direct picture of the plasma dynamics is necessary in order to clarify the hot electron problem. In this study, a plasma diagnosis method was used for the Io plasma torus EUV spectra taken from the Cassini spacecraft. Agreement with previous observations confirmed the background electron temperature and ion compositions as determined by our model. In addition, the available data are matched even better when the model is run with a hot electron component. This consistent confirmation by remote sensing is a first. Because of the limited temporal resolution and observational coverage, the results could not be used to explain the generation process of the hot electrons. However, we expect that this method will be useful in studying the hot electron generation process when data from future missions with better temporal resolution and more complete coverage become available.

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