Hansen, Candice J听1听;听Esposito, Larry W听2听;听Stewart, A Ian听3听;听Meinke, Bonnie K听4听;听Wallis, B听5听;听Colwell, Joshua E听6听;听Hendrix, Amanda R听7听;听, et al.听8
4听Presenting Author
1听Jet Propulsion Laboratory/California Institute of Technology
2听Laboratory for Atmospheric and Space Physics, University of Colorado, 葫芦娃视频
3听Laboratory for Atmospheric and Space Physics, University of Colorado, 葫芦娃视频
4听Laboratory for Atmospheric and Space Physics, University of Colorado, 葫芦娃视频
5听Jet Propulsion Laboratory/California Institute of Technology
6听Planetary Sciences Group, University of Central Florida
7听Jet Propulsion Laboratory/California Institute of Technology
8
In 2005, observations of Saturn鈥檚 moon Enceladus with the Cassini spacecraft revealed a plume of water vapor spewing from the moon鈥檚 south pole (Hansen et al., 2006). The Cassini Ultraviolet Imaging Spectrograph (UVIS) observed an occultation of zeta Orionis by Enceladus鈥� plume in October 2007. This observation resulted in new data on the structure, composition, and water vapor flux of the plume. We detected four high-density gas jets in Enceladus鈥� water vapor plume that are consistent with the dust jets鈥� locations as observed in visible images (Spitale and Porco, 2007). Distinct separation of the two strongest absorption features due to the jets in the occultation profile constrains the ratio of the jets鈥� thermal velocity to vertical velocity to 0.65 +/- 0.1, which means the jets escape the ground at supersonic speeds. In addition, data from the 2007 observation sets a maximum water column density in the plume at ~3 x 1016听肠尘-2, approximately twice the density observed by UVIS in 2005 at the same altitude in the plume (15 km). The comparison of densities in 2005 and 2007 does not agree with the model of tidally-driven compression and tension controlling plume activity-level by opening and closing fissures (Hurford et al., 2007). Another significant result from this observation is the composition of the plume, which reflects the geochemistry of Enceladus鈥� interior. UVIS constrained the Ion and Neutral Mass Spectrometer (INMS) detection of a species with a mass of 28 amu (Spencer et al, 2006), which could be N2听or CO. UVIS did not observe absorption due to CO in 2005 or 2007, excluding 3% CO in the plume at the 2-sigma level.
Hansen, C. J. et al., 2006, Enceladus' water vapor plume: Science, v. 311, p. 1423鈥�1425.
Hurford, T. A., Helfenstein, P., Hoppa, B. V., Greenberg, R. & Bills, B., 2007, Eruptions arising from tidally controlled periodic openings of rifts on Enceladus: Nature, v. 447, p. 292鈥�294.
Spencer, J. R. et al., 2006, Cassini encounters Enceladus: Background and the discovery of a south polar hot spot: Science, v. 311, p. 1401鈥�1405.
Spitale, J. N. & Porco, C. C., 2007, Association of the jets of Enceladus with the warmest regions on its south-polar fractures: Nature, v. 449, p. 695鈥�697.