31st Annual Meeting of the DPS, October 1999
Session 64. Venus
Contributed Oral Parallel Session, Friday, October 15, 1999, 8:30-9:40am, Sala Plenaria

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[64.05] Cassini Ultraviolet Imaging Spectrometer Observations of the Venus Dayglow

A.I.F. Stewart, L.W. Esposito, C.A. Barth, J.E. Colwell, G.M. Lawrence, W.E. McClintock, W.R. Pryor (LASP, University of Colorado), H.U. Keller, A. Korth, H. Lauche (Max-Planck-Institut fur Aeronomie), M.C. Festou (SWRI Boulder), A.L. Lane, C.J. Hansen, J.N. Maki, R.A. West (Jet Propulsion Laboratory), H. Jahn, R. Reulke, K. Warlich (DZLR, Institut fur Weltraumsenorik), D.E. Shemansky (Dept of Aerospace Engineering, USC), Y.L. Yung (Division of Geological and Planetary Sciences, Caltech)

On 24 June 1999 the Cassini spacecraft passed within 600 km of the surface of Venus. The line-of-sight of the Ultraviolet Imaging Spectrometer (UVIS) crossed the dark limb near latitude 30N and SZA 100 deg just before dawn, and the bright limb near latituse 5S and SZA 70 deg just before noon. 55 extreme (56-118 nm) and far (112-191 nm) ultraviolet spectra were acquired in 29 mins. 25 of these contained the dayside airglow. The nominal spectral resolution was 0.24 nm. Prominent features in the FUV spectra include HI 121.6 nm, OI 130.4 and 135.6 nm, CI 156.1 nm and 165.7 nm, and the CO Fourth Positive bands, in which bands of the v' = 0 through 8 and v' = 14 progressions are detectable. Weaker features of NI, CI, CII, OI, and CO are also present. The EUV spectra contain well-defined features at HeI 58.4 nm, OII 83.3 nm, OI 98.9 nm, and HI 102.6 nm. Weaker emissions include OI 104.1 nm, CO (C-X) 108.8 nm, NI 113.5 nm, and a blend of CO (B-X) and OI near 115 nm. The prominent features reported by Stern et al. (Icarus 122, 200-204, 1996) near 87, 90, 94, and 110 nm do not appear in the UVIS spectra.

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