Comparison of Recent Cassini UVIS Observations of Saturn H2 Dayglow Emission

Details Comparison of Recent Cassini UVIS Observations of Saturn H2 Dayglow Emission Comparison of Recent Cassini UVIS Observations of Saturn H2 Dayglow Emission

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p11c0127h&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #P11C-0127

Physics

0355 Thermosphere: Composition And Chemistry, 5704 Atmospheres (0343, 1060), 5709 Composition (1060), 5729 Ionospheres (2459), 6275 Saturn

Scientific paper

A comparative analysis of the Cassini UVIS Saturn H2 dayglow observations is presented. The first spectrum was obtained during the Cassini pre-SOI period by binning multiple Saturn observations from April 2, 2004 to May 12, 2004, at a latitude of 14o S. This spectrum is compared to a recent dayglow spectrum obtained on May 5, 2005, 22 days after the first Cassini UVIS stellar occultation of the Saturn atmosphere. Strong variability in dayglow brightness, not recognized in previous observations, is inferred. The H2 emission is examined for both the EUV and FUV instruments, covering a spectral range of ~(561 to 1900) Å, using a rotational-level, hydrogen physical chemistry model. Details of non-LTE H2 (v : J) partitioning and atmospheric composition predicted from the model are discussed for the range of explored thermospheric altitudes. The competition of solar input (solar photons + photoelectrons) and magnetospheric energy deposition in the thermosphere is examined for both time periods. The determination of deposition rates from the dayglow compared to the requirements derived from the kinetic temperature profile (Hallett et al., Shemansky et al., 2005) will constrain the role of electron impact dissociation of H2 in heating the upper thermospheres of the giant outer planets.

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