Other
Scientific paper
Aug 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993icar..104..324b&link_type=abstract
Icarus (ISSN 0019-1035), vol. 104, no. 2, p. 324-336.
Other
28
Mars Atmosphere, Occultation, Ozonometry, Solar Eclipses, Ultraviolet Spectrometers, Middle Atmosphere, Soviet Spacecraft, Vertical Distribution
Scientific paper
The vertical structure of ozone in the middle atmosphere of Mars is investigated on the basis of solar occultation measurements from the Phobos spacecraft. Ozone is firmly detected in one case, with well correlated evolutions of signals at 270, 277, and 283 nm, about 10 sec before the loss of pointing occurs. Similar profiles are obtained in two other cases, although being more dependent on pointing corrections. When ozone is observed, the ozone number density increases regularly below 55 km altitude to about (0.9 +/- 0.3) x 10 exp 8/cu cm around 42-45 km altitude. The average scale height of the ozone profile above 45 km is 6 +/- 2 km. When ozone is not detected, which implies an ozone concentration lower than about 2 x 10 exp 7/cu cm, the weak abundance of ozone can be easily reproduced by using the thermal structure and humidity conditions derived from the analysis of the clouds, except that the clouds, observed in about 15 percent of cases, are not systematically present in this case.
Blamont E. J. E. J.
Chassefiere Eric
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