Near-resonant energy transfer from vibrationally excited OH(v), v = 9, 8, 1 to CO2

Details Near-resonant energy transfer from vibrationally excited OH(v), v = 9, 8, 1 to CO2 Near-resonant energy transfer from vibrationally excited OH(v), v = 9, 8, 1 to CO2

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008georl..3518102b&link_type=abstract

Geophysical Research Letters, Volume 35, Issue 18, CiteID L18102

Mathematics

Probability

2

Atmospheric Composition And Structure: Middle Atmosphere: Composition And Chemistry, Atmospheric Composition And Structure: Middle Atmosphere: Energy Deposition (3334), Atmospheric Composition And Structure: Airglow And Aurora

Scientific paper

The transfer of vibrational energy from chemiluminescent OH, produced predominately by the H + O 3 -> OH (v) + O 2 reaction, is of importance in modeling the airglow from the atmospheres of Earth, Mars, and Venus. We have calculated the energy transfer probability per collision as function of temperature for the near-resonant processes OH (v) + CO 2 (00001) -> OH(v - 1) +CO 2 (mnpqr) for v = 1, 8, and 9 in the 100 - 350 K temperature range. We show that the measured room temperature values of the removal rate coefficient of OH(v = 9, 8) and OH(v = 1) by CO2, are in agreement with the ones calculated for the vibration-to-vibration (VV) energy transfer (ET) processes OH (v) + CO 2 (00001) -> OH (v - 1) + CO 2 (00011) and OH (1) + CO 2 (00001) -> OH (0) + CO 2 (1001 n) n =1, 2, respectively. The emission from the latter levels of CO2 in the terrestrial mesosphere is not self-absorbed leading to the possibility that these levels may be important contributors to the 4.3 μm emission. Our calculation favors the ``Collisional Cascade'' model of vibrational energy transfer from OH to CO2 that predicts about 50 times more radiation in the Martian Meinel bands over that predicted by the ``Sudden Death'' model. These two models of Martian atmosphere predict vastly different steady-state populations of the vibrational levels of OH and should, because of the chemical reactions, of other trace species, e.g., H, O, and CO, as well.

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