Welcome to the UVIS Team Web Site (Intranet)
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
- 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
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
June 27, 2006