Physics
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p51b1197j&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #P51B-1197
Physics
6005 Atmospheres (1060), 6060 Radiation And Chemistry, 6295 Venus
Scientific paper
Retrievals of trace gas abundances deep in Venus' atmosphere are best achieved by observing the nightside of Venus between 0.8 and 2.5 microns. At high spectral resolution, it is possible to obtain H2O, CO, SO2, CO, OCS, HCl and HF abundances. Accurate synthetic spectra are necessary to assess how the emission spectrum in this region is affected by abundances of these gases. We have developed a very detailed line-by-line computer code that accounts for the non-Lorentzian nature of CO2 and H2O lines far from line centers in this region, and line mixing within the P, Q, and R branches of the 15 micron CO2 band. In addition, we are developing a highly adjustable correlated-k scheme for calculating absorption coefficients that can approach the accuracy of line-by-line calculations. We will show synthetic spectra of the Venus atmosphere in emission from 0.8 to 2.5 microns, and demonstrate the sensitivity of outgoing flux to changes in trace gas abundances. Results for line-by-line and correlated-k calculations will be compared.
Bullock Mark Alan
Jessup Kandis
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