Fine-structure physical chemistry modeling of Uranus H2 X quadrupole emission

Details Fine-structure physical chemistry modeling of Uranus H2 X quadrupole emission Fine-structure physical chemistry modeling of Uranus H2 X quadrupole emission

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005georl..3202204h&link_type=abstract

Geophysical Research Letters, Volume 32, Issue 2, CiteID L02204

Physics

3

Atmospheric Composition And Structure: Ion Chemistry Of The Atmosphere (2419, 2427), Atmospheric Composition And Structure: Thermosphere: Energy Deposition (3369), Planetary Sciences: Fluid Planets: Atmospheres (0343, 1060), Planetary Sciences: Fluid Planets: Ionospheres (2459), Planetary Sciences: Solar System Objects: Uranus

Scientific paper

A new hydrogen physical chemistry model has been developed at the fine-structure level for application to the giant outer planet thermospheres. The model is applied to Uranus because observations of dayglow H2 X 1Σg+ (v) quadrupole and H3+ vibration-rotation emission made at NASA IRTF and UKIRT provide critical constraints for thermospheric modeling. The observed H3+ vibration-rotation emission infers an H3+ dominant ionosphere, predicted only for non-LTE H2 X (v : J). Excitation mechanisms explored are solar and non-solar electron energy deposition. Non-solar electron forcing is constrained by the EUV H2 Lyman and Werner band emission measured by Voyager UVS. Analysis indicates that non-solar electrons are dominant in the energy budget required to predict the observed thermospheric temperature profile. The modeled H2 X quadrupole emission infers that an additional mechanism is required to excite the H2 X (v = 1) population. Non-thermal H produced in dissociative excitation of H2 X is a primary candidate.

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