Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.3103f&link_type=abstract
American Astronomical Society, DPS meeting #39, #31.03; Bulletin of the American Astronomical Society, Vol. 39, p.472
Astronomy and Astrophysics
Astronomy
Scientific paper
Infrared AOTF spectrometer is a part of SPICAM experiment onboard Mars-Express mission. The instrument has a capability of solar occultations and operates in the range 1-1.7 μm with spectral resolution of 3.5 cm-1. FOV of the solar channel is 4.2 arcmin that corresponds to vertical resolution <3.5 km providing the distance to limb does not exceed than 3000km. During the two Martian years about 300 successful infrared occultations have been carried out, with Ls varying from 139° to 344°. We report the results obtained during 25 orbits in MY28 at Ls 130-160, and the latitude range of 40°-55°N. For these orbits, simultaneous observations of atmospheric density from 1.43 μm CO2 band, water vapor mixing ratio based on 1.38 μm absorption, and aerosol opacities were retrieved. Aerosol vertical extinction profiles were obtained at 10 wavelengths in the altitude range from 10 to 60 km. The number density is found to be of the order or below 1cm-3 at the altitudes between 15 and 30 km, with the effective particle radius reff 0.5-1μm. The aerosol haze top altitude does not exceed 40km, except the orbits obtained in the range of 320°-50° degrees of east longitude. In these orbits high-altitude clouds at 50-60km were detected with reff=0.1-0.3μm, variance veff=0.2-0.3μm, and number density N 10cm-3. These clouds are poorly detectable in nadir or ground-based observations, as their vertical optical depth does not exceed 0.01 at 1.1μm. The gas density of the atmosphere were retrieved from CO2 band in the altitude range of 10-90km, and H2O mixing ratio was determined at the altitudes from 15 to 50 km. Unless very high supersaturation of water vapor occurs in the Martian atmosphere, the H2O mixing ratio indicates by about 10K warmer atmosphere at these altitudes than predicted by most of GCM simulations.
Belyaev Dmitry
Bertaux J. J.
Fedorova Anna
Korablev Oleg
Montmessin Franck
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