Physics
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.......40k&link_type=abstract
EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #40
Physics
Scientific paper
The Pioneer Venus Orbiter Infrared Radiometer, ǒrtex, and Venera 15 Fourier Transform Spectrometer, ěnera, observations of thermal emission from Venus' middle atmosphere between 10 degS and 50 degN were used to determine global maps of temperature, cloud optical depth and water vapour abundance. The spectral regions observed include the strong 15 μm carbon dioxide band and the 45 μm fundamental rotational water band. The different spatial and spectral resolution of the two instruments has necessitated the development of flexible and sophisticated analysis tools. New radiative transfer and retrieval models have been developed for this purpose based on correlated-k absorption tables calculated with up-to-date spectral line data. The joint analysis of these two sets of observations has hence been possible for the first time. From the ǒrtex observations, the cloud-top unit optical depth pressure showed a minimum of ˜110±10 mbars in the evening equatorial region and a maximum of ˜160±12 mbars in the morning mid-latitude regions. From the ěnera spectra, the cloud-top pressure was found to increase from morning values of ˜120±10 to 200±30 mbars in the late afternoon/early evening region. The cloud-top water vapour abundances observed by the ǒrtex instrument were found to fluctuate from 10±5 ppm at night up to 85-95±15 ppm in the equatorial cloud-top region shortly after the sub-solar point. The mean ěnera water vapour abundances were found to be of the order of 10±3 ppm with only slight enhancement over the equatorial latitude bands and no clear day-night distinction. The common analysis of these two sets of observations broadly validates previously published individual findings. The differences in the retrieved atmospheric state can no longer be attributed to radiative transfer modelling bias, and suggest significant temporal variability in the middle atmosphere of Venus.
Irwin Patrick G. J.
Koukouli Mary E.
Taylor Fred W.
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