HR: 0800h
AN: P11A-0965    [Abstracts]
TI: Latitudinal Distribution and Seasonal Behavior of Mars Ozone from Infrared Heterodyne Spectroscopy
AU: Fast, K E
EM: kelly.e.fast@nasa.gov
AF: NASA Goddard Space Flight Center, Code 693 NASA Goddard Space Flight Center, Greenbelt, MD 20771 United States
AU: Kostiuk, T
EM: theodor.kostiuk.1@nasa.gov
AF: NASA Goddard Space Flight Center, Code 693 NASA Goddard Space Flight Center, Greenbelt, MD 20771 United States
AU: Annen, J
EM: john.annen@nasa.gov
AF: NASA Goddard Space Flight Center, Code 693 NASA Goddard Space Flight Center, Greenbelt, MD 20771 United States
AU: Espenak, F
EM: fred.espenak@nasa.gov
AF: NASA Goddard Space Flight Center, Code 693 NASA Goddard Space Flight Center, Greenbelt, MD 20771 United States
AU: * Sonnabend, G
EM: samstag@ph1.uni-koeln.de
AF: NAS/NRC/GSFC, Code 693/NRC NASA Goddard Space Flight Center, Greenbelt, MD 20771 United States
AU: Livengood, T A
EM: tlivengood@challenger.org
AF: Challenger Center, 1250 North Pitt St., Alexandria, VA 22314 United States
AU: Hewagama, T
EM: tilak@cuzco.gsfc.nasa.gov
AF: University of Maryland, College Park, Department of Astronomy University of Maryland, College Park, MD 20742-2421 United States
AU: A'Hearn, M F
EM: ma@astro.umd.edu
AF: University of Maryland, College Park, Department of Astronomy University of Maryland, College Park, MD 20742-2421 United States
AB: Ozone is an important tracer of the photochemical processes responsible for the stability of Mars' CO$_2$ atmosphere. Infrared heterodyne spectroscopy with a resolving power of $1-5 x 10^6$ has been used to directly measure fully-resolved lineshapes of Mars atmospheric O$_3$ features from the ground. Observations at 9.6 microns have been made at Mars apparitions from 1988 through 2003 to directly measure O$_3$ as various latitudes and local times. Carbon dioxide features are also present in the bandpass, providing temperature constraints during the radiative transfer analysis of the O$_3$ lines. We present ozone abundance as a function of latitude for various Mars seasons (L$_S$ = 40, 73, 102, 115, 202, 204, 291). The latitudinal behavior of the ozone is compared to that of water taken close in time in order to investigate the anti-correlation predicted by photochemistry. This work was supported by the NASA Planetary Astronomy Program.
DE: 5405 Atmospheres--composition and chemistry
DE: 5494 Instruments and techniques
DE: 6225 Mars
DE: 0343 Planetary atmospheres (5405, 5407, 5409, 5704, 5705, 5707)
SC: Planetary Sciences [P]
MN: 2004 AGU Fall Meeting