2-D Maps Of The O2(1Δ) Emission During The Mars Pre-aphelion Season

Details 2-D Maps Of The O2(1Δ) Emission During The Mars Pre-aphelion Season 2-D Maps Of The O2(1Δ) Emission During The Mars Pre-aphelion Season

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.0607n&link_type=abstract

American Astronomical Society, DPS meeting #40, #6.07; Bulletin of the American Astronomical Society, Vol. 40, p.396

Astronomy and Astrophysics

Astronomy

Scientific paper

We have constructed 2-D maps of the O2 (1Δ) emission (near 1.27 µm wavelength) for four dates spanning the pre-aphelion season on Mars. This emission can be used as an indicator of ozone above 20 km. Results will be presented for Ls = 333o (Jan 13, 2004), Ls = 357o (Jan 16, 2006), Ls = 20o (Jan 19, 2008), and Ls = 50o (Mar 27, 2008).
The data were collected using CSHELL at the NASA Infrared Telescope Facility. The slit was positioned in the North-South direction on Mars. Spectral/spatial data were taken at 1.0 arc-sec increments East to West across Mars. For Ls = 333o, no emissions were detected above the noise level (0.2 MegaRayleighs, MR). Just before the vernal equinox (Ls = 357o), strong emissions (> 12 MR) were detected in both polar-regions. At Ls = 20o, emissions were still strong in the polar-regions, with no detections in the middle to low latitudes. For Ls = 50o, emissions (strong in the polar regions and weaker in the mid- and low-latitudes) occurred across the planet. All detected emissions showed a strong diurnal variation that peaks near mid-day and is weak during early morning and late afternoon local time.
Central meridional maps for these dates will be compared to results taken near aphelion at Ls = 67o (Jan 21, 1997) (Novak et al. 2002). The O2 (1Δ) state originates from the photolysis of ozone. This state is quenched by carbon dioxide at low altitudes; the quenching is weak above 20 km. As Mars approaches aphelion, the atmosphere cools causing the water vapor to exist mainly at lower altitudes, permitting ozone to persist at higher altitudes.
We acknowledge support from NSF RUI Program (AST-0505765) and NASA's Planetary Astronomy Program.

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