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Scientific paper
May 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.1306s&link_type=abstract
American Astronomical Society, 192nd AAS Meeting, #13.06; Bulletin of the American Astronomical Society, Vol. 30, p.838
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1
Scientific paper
High-Resolution Study of New Terrestrial Nightglow Features - Beyond OH T. G. Slanger, P. C. Cosby, and D. L. Huestis, Aeronomy Group, Molecular Physics Laboratory, SRI International, Menlo Park, CA 94025 and D. E. Osterbrock and J. P. Fulbright, University of California Observatories/Lick Observatory, University of California, Santa Cruz, CA 95064 Sky spectra taken with the HIRES echelle spectrometer on the Keck I telescope on Mauna Kea have led to the discovery of an impressive array of new spectral nightglow features, belonging to the O2(b(1) Sigma_ {g}(+) - X(3}/Sigmag({-)) ) Atmospheric Band system. The previous record for rotationally-resolved spectroscopy in this system has long been held by Babcock and Herzberg (1948), who detected the b(1) Sigma_ {g}(+) state up to v = 3 in solar absorption spectra. Recently, Osterbrock et al. (1996) have published 0.2- Angstroms resolution sky spectra showing levels up to v = 4, and these same data have been further analyzed to reveal that levels up to v = 10 could be seen. With a more recent data set in which signals have been accumulated for up to 120 hours, we are now able to measure levels up to v = 15, which encompasses 3/4 of the b(1) Sigma_ {g}(+) state potential. The discovery of these new spectral features in the O2 terrestrial nightglow has an impact on our understanding of other planets. The b(1) Sigma_ {g}(+) state, along with the lower-lying a(1) Delta_ {g} state, produces emission which should be discernible in the CO2 atmospheres of Mars and Venus, as a result of the oxygen-atom recombination which is recognized to be as important a process in those environments as in the terrestrial atmosphere. The a(1) Delta_ {g} state emission, from the v = 0 level, is a well-known though puzzling feature of the Venus atmosphere, both on the day and night sides. From the HIRES observations, and our laboratory program to determine the temperature-dependent effects of atmospheric quenching of vibrationally-excited levels by O2, N2, and CO2, we ultimately expect to be able to predict the intensities to be found on Mars and Venus in these O2 emission systems.
Cosby Philip C.
Fulbright Jon P.
Huestis David L.
Osterbrock Donald E.
Slanger Tom G.
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