Physics
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusm.p31a..02k&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #P31A-02
Physics
5405 Atmospheres (0343, 1060), 5410 Composition (1060, 3672), 6225 Mars
Scientific paper
The O2 dayglow at 1.27 μm is a sensitive tracer of photochemistry on Mars. Ground-based mapping of the O2 dayglow was made using a high-resolution long-slit spectrograph CSHELL at NASA IRTF. The observations were conducted in the period of 1997 to 2006 and cover seven seasons that are uniformly spread over the martian year (LS = 10, 67, 112, 148, 173, 247, and 312°). The previously reported results covered LS = 67, 112, 148, and 173° (Krasnopolsky, Icarus 165, 315-325, 2003). The measured dayglow intensities have been corrected for the instrument point spread function, martian airmass, and the surface reflectivity. The dayglow intensities at low latitudes are maximal at 7 MR near aphelion and diminish to 3-2 MR in northern summer and then to 1 MR near perihelion (southern summer). Latitudinal variations are significant but much smaller than those expected for the anticorrelation with water vapor. Currently this is the most extended observational database on the photochemical products on Mars. Mapping of the CO mixing ratio on Mars is made using observations of some lines of the (3-0) band at 1.57 μm and nearby CO2 lines with the same instrument. The previously published observations at LS = 112° showed no variations of the CO mixing ratio with local time and elevation and revealed a significant north-south asymmetry which is caused by condensation/sublimation of CO2 on the polar caps (Krasnopolsky, JGR 108, E2, 5010, 2003). Later a similar phenomenon was observed for Ar by the Mars Odyssey (Sprague et al., Science 306, 1364-1367, 2004). Here we report and discuss observations of this asymmetry at LS = 10, 173, and 312°. This new phenomenon is related to the atmospheric dynamics and polar processes and should be simulated by GCM's.
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