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UVIS header

Welcome to the UVIS Team Web Site (Intranet)

Site Map

Cassini Press Archives (links to public press archive page)


Public Fileshare Page: You can post files on this page for people to download outside of this password-protected site. Send your files to me and I'll post them on the public fileshare page for a period of time. The page is part of the Public UVIS site. However, it is "hidden" and isn't linked from any page on the public site (since the files are not otherwise meant for the general public). So, tell people to go to the UVIS home page and type "fileshare" at the end of the URL to get to the fileshare page: http://lasp.colorado.edu/cassini/fileshare

UVIS Scientific Objectives

The scientific purpose of the UVIS investigation is to explore all aspects of the Saturn system that reveal themselves in ultraviolet light. These include composition and temperature of the atmospheres of Saturn and Titan; the spectral reflectance and albedos of the rocky and icy moons; the gross and fine structure of Saturn's ring system; its response to variations in the solar wind; and the abundance of deuterium in Titan's atmosphere.

  • Atmospheres:   UVIS will observe both the airglows and solar reflectances of the atmospheres. The solar reflectances reveal the presence of gases through their absorption spectra, while the airglow contains the emission spectra of gasses excited by EUV sunlight and auroral presentation. Of particular interest are hydrocarbons including methane, acetylene and ethylene on both Saturn and Titan and nitrogen and carbon species on Titan
  • Satellites:   Sunlight reflected from rocky and icy surfaces contain absorption spectra characteristic of surface minerals and gasses trapped in ices, such as water and carbon dioxide.

  • Rings:   The rings can be observed in both reflected and transmitted sunlight. These observations yield information about the composition optical depth and sizes of the ring particles. The ring structure at very high resolution can be obtained by observing the light from bright stars as they are occulted by the rings. This is done using a high-speed ultraviolet photometer.

  • Solar wind response:   Saturn's magnetosphere responds to variations in solar wind pressure, which cause perturbations in the planet's magnetic field. In consequence, variations in auroral activity occur and these can be observed by UVIS.

  • Deuterium:   UVIS includes hydrogen and deuterium absorption cells with which the abundance of deuterium on Titan and Saturn can be determined.


Feedback, changes and additions:
iIf you have any suggestions, find problems, or you would like to add your own routines, publications, or other documentation to the collections, please contact Laura Bloom.



Page updated June 27, 2006

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