Resolving the mesospheric nighttime 4.3 µm emission puzzle: comparison of the CO 2 ( ν 3 ) and OH( ν ) emission models

In the 1970s, the mechanism of vibrational energy transfer from chemically produced OH(nu) in the nighttime mesosphere to the CO2(nu(3)) vibration, OH(nu) double right arrow N-2(nu) double right arrow CO2(nu(3)), was proposed. In later studies it was shown that this "direct" mechanism for simulated nighttime 4.3 mu m emissions of the mesosphere is not sufficient to explain space observations. In order to better simulate these observations, an additional enhancement is needed that would be equivalent to the production of 2.8-3N(2)(1) molecules instead of one N-2(1) molecule in each quenching reaction of OH(nu) + N-2(0). Recently a new "indirect" channel of the OH(nu) energy transfer to N-2(nu) vibrations, OH(nu) double right arrow O(D-1) double right arrow N-2(nu), was suggested and then confirmed in a laboratory experiment, where its rate for OH(nu = 9) + O(P-3) was measured. We studied in detail the impact of the "direct" and "indirect" mechanisms on CO2(nu(3)) and OH(nu) vibrational level populations and emissions. We also compared our calculations with (a) the SABER/TIMED nighttime 4.3 mu m CO2 and OH 1.6 and 2.0 mu m limb radiances of the mesosphere-lower thermosphere (MLT) and (b) with ground-and space-based observations of OH(nu) densities in the nighttime mesosphere. We found that the new "indirect" channel provides a strong enhancement of the 4.3 mu m CO2 emission, which is comparable to that obtained with the "direct" mechanism alone but assuming an efficiency that is 3 times higher. The model based on the "indirect" channel also produces OH(nu) density distributions which are in good agreement with both SABER limb OH emission observations and ground and space measurements. This is, however, not true for the model which relies on the "direct" mechanism alone. This discrepancy is caused by the lack of an efficient redistribution of the OH(nu)) energy from higher vibrational levels emitting at 2.0 mu m to lower levels emitting at 1.6 mu m. In contrast, the new "indirect" mechanism efficiently removes at least five quanta in each OH(nu >= 5) + O(P-3) collision and provides the OH(nu) distributions which agree with both SABER limb OH emission observations and ground-and space-based OH(nu)) density measurements. This analysis suggests that the important mechanism of the OH(nu)) vibrational energy relaxation in the nighttime MLT, which was missing in the emission models of this atmospheric layer, has been finally identified.