Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p33a1427r&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #P33A-1427
Physics
0310 Airglow And Aurora, 0343 Planetary Atmospheres (5210, 5405, 5704), 6005 Atmospheres (1060), 6009 Aurorae, Airglow, And X-Ray Emission, 6295 Venus
Scientific paper
Ultraviolet nightglow have been detected on Venus for the first time by Barth and al., in 1968, from mariner 5, then identified like to be nitric oxide nightglow by Feldmann and al., and by Stewart and Barth, in 1979, with Pioneer. SPICAV (SPectroscopy for the Characteristics of the Atmosphere of Venus), currently in fly on board Venus Express, also see them. We descibe here a direct model allowed to reproduce this nitric oxide nightglows. It is a first approach in a better understanding of the dynamic phenomena of the venusian thermosphere. This nightglows are due to radiative recombinaison process. On the dayside of the planet, we have nitrogen and oxygen atoms created by UV disssociation of N2, CO2 and O2. This atoms are transported on the nightside, where they recombine themselves and emit an ultraviolet radiation. Thus NO nightglow are tracers of the descending branch of the solar, anti-solar circulation in the thermosphere of Venus. The model using geometric parameters who are fixed for each observation, simulate the travel of a ray of light inside the spectrometer and reproduce the spectra of nightglows. We model a nitric oxide layer, controled by his borderline altitudes and his brightness. Wa have to adjust the parameters of the layer to fit the data. The results, in the making, already are very supporting. Thus, fit the ultraviolet nitric oxide nightglows, as a tracer of the venusian thermospheric circulation, will lead to a better understanding of the dynamic phenomena in the same region of this atmosphere.
Bertaux J. J.
Montmessin Franck
Royer Emmanuel
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