Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p33a0235s&link_type=abstract
American Geophysical Union, Fall Meeting 2005, abstract #P33A-0235
Physics
5405 Atmospheres (0343, 1060), 6295 Venus
Scientific paper
Venus Express is scheduled to arrive at Venus in April, 2006, and atmospheric emissions will be studied with the SPICAV/SOIR spectrometer, which is similar to the SPICAM spectrometer on board the Mars Express orbiter. Because both atmospheres are predominantly CO2/N2, it is expected that emissions in the UV will be similar. Mars Express has already shown that the predominant 200-300 nm nightglow emission is from excited states of NO, as is known for Venus from the Pioneer Venus mission. From Mars Express, the presence of O(1S) from its nightglow emission at 297.2 nm is somewhat ambiguous, although in the dayglow this emission is strong, as shown earlier by the Mariner missions. Because it is now known that Venus O(1S-1D) emission at 557.7 nm can be as strong as the terrestrial green line, although very variable, we expect that Venus Express will be able to make observations of the O(1S-3P) 297.2 nm line, and measure its seasonal and spatial variations. The SOIR instrument measures the IR emissions to a blue cut-off of 700 nm. Thus, it is hoped that emission of the O2 Atmospheric 0-0 band at 762 nm is discernible, as well as the weak O2 Herzberg II and Chamberlain bands above 700 nm. The very variable O2 IR Atmospheric 0-0 band emission at 1270 nm should be easily observable.
Sharpee Brian D.
Slanger Tom G.
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