The mechanism of the air-afterglow NO + O → NO2 + hν

Becker, K. H.; Groth, W.; Thran, D.

doi:10.1016/0009-2614(72)80152-0

Cited by 79 publications

(28 citation statements)

References 19 publications

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“…(b) A separate test carried out herein of replacing the surface with a beam of NO produced no observable twobody, gas-phase emissions. This last result is consistent with the measured rate constant for the reaction NO+ 0~NO2 of 4.2 X 10 cm /moleculesec reported by Seeker, Qroth, and Thran [19]. Under present conditions of NO and 0-atom density, this would correspond to -10 recombinations/cm sec, an amount that would be undetected.…”

Section: Chemiluminescence Spectrasupporting

confidence: 92%

Recombination of 5-eV O(3P) atoms with surface-adsorbed NO: Spectra and their dependence on surface material and temperature

et al. 1992

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Recombination spectra are measured in the wavelength range 300 -850 nm resulting from collisions of 5-eV 0('P) atoms with NO adsorbed on MgF2, Ni, and Ti surfaces. The dependence of the chemiluminescence intensity on surface temperature (240-340 K) is measured, and activation energies for desorption of the physisorbed NO obtained. Activation energies as a function of wavelength for each material are also reported. It is found that, with minor variations, the recombination spectra are similar for the three surfaces, and that the emitter is very likely electronically excited NO2. All three materials exhibit a greater tendency to emit at the lower temperatures. MgFz has the greatest tendency to chemiluminesce, followed by Ni then Ti. Also, the activation energies for NO desorption are similar for the surfaces, and are independent of emission wavelength. The results are interpreted as a single mechanism of removal, with increasing T, of physisorbed NO from saturated surfaces of different coverage.PACS number(s): 79.20.Nc, 68.10.Jy

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Section: Chemiluminescence Spectrasupporting

confidence: 92%

Recombination of 5-eV O(3P) atoms with surface-adsorbed NO: Spectra and their dependence on surface material and temperature

et al. 1992

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“…(4) for calculating k λ , the total bimolecular rate coefficient for the NO 2 chemiluminescence. Becker et al (1972), including the temperature dependence of the three-body reaction, F 3 (T ), reported by Whytock et al (1976) and the possible temperature dependence of the two-body reaction, F 2 (T ), suggested by Sharp (1984), as…”

Section: No From the Photometric Measurementsmentioning

confidence: 98%

“…Becker et al, 1972). At high altitudes (low pressure), the chemiluminescence is believed to arise solely from the two-body radiative recombination reaction:…”

Section: No From the Photometric Measurementsmentioning

confidence: 99%

Observations of NO in the upper mesosphere and lower thermosphere during ECOMA 2010

et al. 2012

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Abstract. In December 2010 the last campaign of the German-Norwegian sounding rocket project ECOMA (Existence and Charge state Of Meteoric smoke particles in the middle Atmosphere) was conducted from Andøya Rocket Range in northern Norway (69 • N, 16 • E) in connection with the Geminid meteor shower. The main instrument on board the rocket payloads was the ECOMA detector for studying meteoric smoke particles (MSPs) by active photoionization and subsequent detection of the produced charges (particles and photoelectrons). In addition to photoionizing MSPs, the energy of the emitted photons from the ECOMA flash-lamp is high enough to also photoionize nitric oxide (NO). Thus, around the peak of the NO layer, at and above the main MSP layer, photoelectrons produced by the photoionization of NO are expected to contribute to, or even dominate above the main MSP-layer, the total measured photoelectron current. Among the other instruments on board was a set of two photometers to study the O 2 (b 1 + g − X 3 − g ) Atmospheric band and NO 2 continuum nightglow emissions. In the absence of auroral emissions, these two nightglow features can be used together to infer NO number densities. This will provide a way to quantify the contribution of NO photoelectrons to the photoelectron current measured by the ECOMA instrument and, above the MSP layer, a simultaneous measurement of NO with two different and independent techniques. This work is still on-going due to the uncertainties, especially in the effort to quantitatively infer NO densities from the ECOMA photoelectron current, and the lack of simultaneous measurements of temperature and density for the photometric study. In this paper we describe these two techniques to infer NO densities and discuss the uncertainties. The peak NO number density inferred from the two photometers on ascent was 3.9 × 10 8 cm −3 at an altitude of about 99 km, while the concentration inferred from the ECOMA photoelectron measurement at this altitude was a factor of 5 smaller.

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“…The OSIRIS [NO] retrieval technique, discussed in more detail by Gattinger et al [2009Gattinger et al [ , 2010 and Sheese et al [2011a], fits a model spectrum [Becker et al, 1972] to the OSIRIS observations of the NO 2 afterglow continuum over the wavelength range 430-810 nm in order to determine the limb radiance profiles. The definitive measurement of the NO 2 afterglow spectral profile made by Becker et al [1972] remains unchallenged, as the reaction vessel they used was unique, being 7.5 m in diameter. They clearly observed a shift of the NO 2 continuum spectral peak with vessel pressure, an effect included in the spectral fitting analysis used in this study.…”

Section: Description Of the [No] Data Sets And Satellite Instrumentsmentioning

confidence: 99%

Odin observations of Antarctic nighttime NO densities in the mesosphere–lower thermosphere and observations of a lower NO layer

et al. 2013

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[1] The Optical Spectrograph and Infrared Imaging System (OSIRIS) on the Odin satellite currently has an eight-year dataset of nighttime Antarctic nitric oxide densities, [NO], in the mesosphere-lower thermosphere (MLT) region. In this work, the OSIRIS data are compared with a similar data set from the Sub-Millimeter Radiometer (SMR), also on the Odin satellite. Both of the Odin data sets are compared with twilight [NO] from the Atmospheric Chemistry Experiment-Fourier Transform Spectrometer (ACE-FTS) on the SciSat-I satellite. Direct comparisons of OSIRIS and SMR profiles show large differences, indicating that the individual [NO] profiles of one or both data sets may not be valid. However, when comparing averaged [NO], variations on timescales of weeks-years in all three data sets are in good agreement and correspond to the 27 day and 11 year solar cycles. The averaged OSIRIS values are typically 10% greater than SMR and 30% greater than ACE-FTS, which are within the estimated OSIRIS systematic uncertainties. These results suggest that the satellite-derived data sets can be used for determining polar-mean NO climatology and variations on timescales of weeks-years. The OSIRIS and SMR nighttime data sets show that the [NO] peak height in the MLT decreases throughout the autumn, from an altitude near or above 100 km to a minimum altitude ranging from 90 to 95 km around winter solstice. A similar decrease in [NO] peak height is observed in modeled NO climatology from the Specified Dynamics-Whole Atmosphere Community Climate Model (SD-WACCM), although the SD-WACCM climatology exhibits a decrease throughout autumn from 107 km down to 102 km. The results suggest that global climate models require more sophisticated auroral forcing simulations in order to reproduce observed NO variations in this region.

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The mechanism of the air-afterglow NO + O → NO2 + hν

Cited by 79 publications

References 19 publications

Recombination of 5-eV O(3P) atoms with surface-adsorbed NO: Spectra and their dependence on surface material and temperature

Recombination of 5-eV O(3P) atoms with surface-adsorbed NO: Spectra and their dependence on surface material and temperature

Observations of NO in the upper mesosphere and lower thermosphere during ECOMA 2010

Odin observations of Antarctic nighttime NO densities in the mesosphere–lower thermosphere and observations of a lower NO layer

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