Physics
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufm.p44a..02h&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #P44A-02
Physics
5704 Atmospheres: Composition And Chemistry, 6275 Saturn
Scientific paper
An analysis of the Cassini UVIS Saturn H2 Lyman and Werner band emission is presented. The spectrum was obtained during the Cassini pre-SOI period by binning multiple Saturn observations from April 2, 2004 to May 12, 2004. The H2 dayglow emission is concentrated near the sub-solar point at a latitude of approximately -21 degrees. The H2 emission is examined for both the EUV and FUV instruments, covering a total spectral range of ˜(561 to 1900) Å. The H2 emission is modeled using fine-structure, hydrogen physical chemistry. The relative contributions of solar and low energy electron excitation in the observed emission are analyzed with the fine-structure chemistry model. H2 solar resonance scattering is more prevalent in the Saturn dayglow spectrum than the Jupiter dayglow spectrum obtained by Cassini UVIS in December of 2000. Details of non-LTE H2 (v : J) partitioning and altitude range of excitation predicted from the hydrogen chemistry model are discussed. The source processes and altitude inferred from the spectrum have important implications for the examination of the Saturn thermospheric heating mechanism.
Cassini UVIS Team
Hallett Janet Tew
Liu Xiandong
Shemansky Don E.
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