Thermal structure and dust loading of the Martian atmosphere during late southern summer - Mariner 9 revisited

Details Thermal structure and dust loading of the Martian atmosphere during late southern summer - Mariner 9 revisited Thermal structure and dust loading of the Martian atmosphere during late southern summer - Mariner 9 revisited

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....98.3261s&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. E2, p. 3261-3279.

Physics

53

Atmospheric Temperature, Dust, Mars Atmosphere, Planetary Meteorology, Summer, Emission Spectra, Optical Thickness, Southern Hemisphere, Thermal Emission, Mars, Temperature, Dust, Loading, Atmosphere, Emissions, Techniques, Spectra, Spacecraft Observations, Iris Instrument, Optical Properties, Mariner 9 Mission, Analysis, Depth, Opacity, Altitude, Abundance, Latitude, Diurnal Variations, Circulation, Polar Region, Procedure, Radiative Transfer, Brightness, Calculations, Pressure, Parameters, Model, Surface,

Scientific paper

Thermal emission spectra recorded by the Mariner 9 IR interferometer spectrometer (IRIS) are used to investigate the temperature structure and dust loading of the Martian atmosphere. The analysis is restricted to a subset of the IRIS data consisting of approximately 2400 spectra in a 12-day period extending from LS of 343 to 348 deg, corresponding to late southern summer on Mars. The largest column-integrated 9-micron dust optical depths (about 0.4) occur over the equatorial regions. The highest atmospheric temperatures (greater than 260 K) are found at low altitudes near the subsolar latitude (about 6 deg S), while the coldest temperatures (less than 150 K) are found at levels near 1.0 mbar over the winter pole. The existence of a net zonally averaged meridional circulation with rising motion at low latitudes, poleward flow at altitudes above 40 km, and subsidence over the poles is suggested.

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