The composition and structure of the Enceladus plume - INMS
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The composition and structure of the Enceladus plume - INMS
Jun 9, 2011 - at the south polar region of Saturn's moon Enceladus. The. Extreme Ultraviolet (EUV) spectrum is dominated by the spectral signature of H2O ...
GEOPHYSICAL RESEARCH LETTERS, VOL. 38, L11202, doi:10.1029/2011GL047415, 2011
The composition and structure of the Enceladus plume C. J. Hansen,1 D. E. Shemansky,2 L. W. Esposito,3 A. I. F. Stewart,3 B. R. Lewis,4 J. E. Colwell,5 A. R. Hendrix,6 R. A. West,6 J. H. Waite Jr.,7 B. Teolis,7 and B. A. Magee7 Received 10 March 2011; revised 20 April 2011; accepted 21 April 2011; published 9 June 2011.
[1] The Cassini Ultraviolet Imaging Spectrograph (UVIS) observed an occultation of the Sun by the water vapor plume at the south polar region of Saturn’s moon Enceladus. The Extreme Ultraviolet (EUV) spectrum is dominated by the spectral signature of H2O gas, with a nominal line‐of‐sight column density of 0.90 ± 0.23 × 1016 cm−2 (upper limit of 1.0 × 1016 cm−2). The upper limit for N2 is 5 × 1013 cm−2, or
