DPS 35th Meeting, 1-6 September 2003
Session 3. Mars Atmosphere I
Oral, Chairs: T. A. Livengood and A. Colaprete, Tuesday, September 2, 2003, 10:30am-12:00noon, DeAnza I-II

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[3.02] The Martian FUV Dayglow Observed by FUSE

G. R. Gladstone, K. D. Retherford, S. A. Stern (SwRI), R. Link (Algoma Research), S. W. Bougher (U. of Michigan)

The Far Ultraviolet Spectroscopic Explorer (FUSE) satellite was used by us to observe Mars on 7/8/2001 for 8030s and on 8/10/2001 for 13240s. During these observations, 6230s and 10990s, respectively, occurred when the satellite was within Earth's shadow and terrestrial airglow contamination was minimized. An earlier observation (Krasnopolsky and Feldman 2002, Icarus, 160, 86) lasted 18340s, of which 10230s were obtained from Earth's shadow. The FUSE spectra cover the wavelength range 90-120~nm, at a resolving power of about 5000, and contain a large number of emission lines of H, He, C, N, O, Ar, N+, C+, and Ar+, as well as bands of N2 and CO, as described by Krasnopolsky and Feldman. Here we present full-disk simulations of several of emission line multiplets, using standard model atmospheres (e.g., Nair et~al. 1994, Icarus, 111, 124; Krasnopolsky 2002, J. Geophys. Res., 107, 5128), to place constraints on disk-averaged abundances of the major species of the upper atmosphere. We gratefully acknowledge support from NASA through FUSE grant NAG5-10920.

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Bulletin of the American Astronomical Society, 35 #4
© 2003. The American Astronomical Soceity.