Physics
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusm.p21b..06s&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #P21B-06
Physics
0310 Airglow And Aurora, 0358 Thermosphere: Energy Deposition, 0360 Transmission And Scattering Of Radiation, 6207 Comparative Planetology, 6280 Saturnian Satellites
Scientific paper
EUV airglow observations of Titan by the Voyager 1 Ultraviolet Spectrometer (UVS) in 1980 indicated that the spectrum between 52-110 nm was excited primarily by electron impact on N2. Since then, our understanding of the various emission features contributing to the observed signal has substantially evolved. High resolution electron impact emission laboratory measurements of the important N2 Carroll-Yoshino (CY) c4'-X (0,v") bands provided constraints on the predissociation yield of the excited c4'(0) state. CY(0,v") is radiatively trapped in Titan's atmosphere so that c4'(0) predissociation is compounded over its optically thin value, increasing the loss to the system. Model results have shown that the depleted CY(0,0) emission near 95.8 nm is redistributed to the more optically thin (0,v">0) bands with some additional loss to the system through extinction. More recently, models of Titan's airglow and observations of the Earth's airglow at high spectral resolution showed the possible significance of many weaker N2 and N I emissions that were unresolved by the UVS at Titan. In this review, we summarize the current understanding of the Titan EUV airglow up until the arrival of Cassini. We outline some questions that remain unanswered, which include, but are not limited to, a possible misidentification of N2 CY(0,0) in the Voyager 1 UVS spectra and a possible auroral contribution to the EUV airglow.
Bishop James
Feldman Paul D.
Stevens Michael Hugh
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