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Atomic oxygen in the Martian thermosphereModern models of thermospheric composition and temperature and of excitation and radiative transfer processes are used to simulate the O I 130-nm emission from Mars measured by the Mariner 9 ultraviolet spectrometer. This paper uses the Mars thermospheric general circulation model calculations (MTGCM) of Bougher et al. (1988) and the Monte Carlo partial frequency redistribution multiple scattering code of Meier and Lee (1982). It is found that the decline in atomic oxygen through the daylight hours predicted by the MTGCM cannot be reconciled with the excess afternoon brightness seen in the data. Oxygen concentrations inferred from the data show a positive gradient through the day, in agreement with the original analysis by Strickland et al. (1973). In addition, the data suggest that the oxygen abundance increases toward high southerly latitudes, in contrast with the MTGCM prediction of high values in the Northern Hemisphere. It appears that solar forcing alone cannot account for the observed characteristics of the Martian thermosphere and that wave and tidal effects may profoundly affect the structure, winds, and composition.
Document ID
19920036859
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Stewart, A. I. F.
(Colorado Univ. Boulder, CO, United States)
Alexander, M. J.
(Colorado, University Boulder, United States)
Meier, R. R.
(U.S. Navy, E.O. Hulburt Center for Space Research, Washington DC, United States)
Paxton, L. J.
(Johns Hopkins University Laurel, MD, United States)
Bougher, S. W.
(Arizona, University Tucson, United States)
Fesen, C. G.
(Dartmouth College Hanover, NH, United States)
Date Acquired
August 15, 2013
Publication Date
January 1, 1992
Publication Information
Publication: Journal of Geophysical Research
Volume: 97
ISSN: 0148-0227
Subject Category
Lunar And Planetary Exploration
Accession Number
92A19483
Funding Number(s)
CONTRACT_GRANT: NAGW-389
Distribution Limits
Public
Copyright
Other

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