Water Vapor Abundances over Mars North High Latitude Regions: 1996-1999

Details Water Vapor Abundances over Mars North High Latitude Regions: 1996-1999 Water Vapor Abundances over Mars North High Latitude Regions: 1996-1999

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icar..154..183s&link_type=abstract

Icarus, Volume 154, Issue 1, pp. 183-189 (2001).

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We present column abundances of water vapor in Mars' atmosphere over high north latitudes for Ls 46°-146° during 1996-1997 and Ls 34°-180° during 1998-1999. These abundances have been obtained by ground-based high-resolving-power spectroscopy in the very near IR (8174-8200 Å) from the 1.5-m Catalina observatory near Tucson, AZ. All of the measurements have been corrected for atmospheric dust opacity, which increases the measured water vapor abundance over the ``apparent measurement'' by appreciable amounts at long path lengths. Dust measurements in 1998-1999 were made by near simultaneous measurements, with the same instrument, of the CO2 absorption lines in the nearby spectral region between 8689 and 8692 Å. We use a doubling and adding radiative transfer code to obtain the dust optical thickness. High northern latitude dust opacities were between 0.8 and 1.0 in this data set for 1998-1999. For the high-latitude measurements made in 1996-1997 during and following observed spring dust storm activity, the dust opacity (τdust=0.8) was adopted. The computations account for the geometry of the observations (incoming airmass, outgoing airmass, and phase angle). Measurements show a strong increase in water vapor abundance from 8 to 76 ppt. μm with onset of spring and early summer (Ls 34°-118°) followed by an abrupt drop to less than 1 ppt. μm by summer's end. .

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