Mechanism of the air afterglow NO+O→NO2+hv

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

doi:10.1016/s0082-0784(73)80035-9

Cited by 19 publications

(23 citation statements)

References 38 publications

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“…The spectral profile, corresponding to mesopause region atmospheric pressure, is slightly different from the low-pressure spectral shape measured in the laboratory by Becker et al [1972]. The shortwave limit of the continuum is approximately 370 nm in agreement with the measurements by Stewart [1957].…”

Section: The Osiris No 2 Continuum Observationssupporting

confidence: 82%

“…The analysis requires knowledge of the spectral distribution and absolute emission efficiency the NO 2 afterglow continuum, available from laboratory measurements by Becker et al [1972] and Whytock et al [1976]. Gattinger et al [2009] [8] Finally, the observations are briefly discussed in section 6 with emphasis on the observed spatial variability of the three components, NO 2 continuum VER, [O], and [NO], and possible source mechanisms.…”

Section: Introductionmentioning

confidence: 99%

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NO₂ air afterglow and O and NO densities from Odin‐OSIRIS night and ACE‐FTS sunset observations in the Antarctic MLT region

et al. 2010

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The continuum spectrum produced by the NO + O(+M) → NO2(+M) + hv chemiluminescent reaction has been detected in the upper mesospheric dark polar regions by Optical Spectrograph and Infra‐Red Imager System (OSIRIS) on the Odin spacecraft. For the sample period of 8–9 May 2005, Southern Hemisphere, limb radiance profiles of continuum spectra, resolved from OH airglow and auroral contamination, are inverted to obtain volume emission rate altitude profiles. The maximum observed differential brightness referred to zenith viewing is 1.2 × 107 photons cm−2 s−1 nm−1 at 580 nm with a measurement uncertainty 5 × 105 photons cm−2 s−1 nm−1, for an analysis range 80–101 km. Atomic oxygen densities [O] required by the analysis to derive NO densities [NO] are determined from OSIRIS O2(b1Σg+ − X3Σg−) 0‐0 band night airglow observations and from Atmospheric Chemistry Experiment‐Fourier Transform Spectrometer (ACE‐FTS) sunset ozone observations. The derived Southern Hemisphere [O] map that shows pronounced longitudinal variation, maximum of 7 × 1011 cm−3, considerably exceeding MSIS model values, and suggests significant dynamical influence. Combining the continuum observations and the derived [O], a hemispheric map of derived [NO] is assembled that also shows considerable spatial variation, maximum of 1.1 × 109 cm−3, measurement uncertainty of 3 × 107 cm−3. Comparing the two maps, the geographical distribution of [NO] differs considerably from that of [O]. From a qualitative comparison, the distribution of derived [NO] is similar to that in coordinated GUVI LBH1 auroral precipitation images. The OSIRIS‐derived [NO] agrees with the measured ACE‐FTS [NO] to within 1 × 108 cm−3. The estimated systematic uncertainty of the NO densities derived from OSIRIS observations is approximately 30%.

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Section: The Osiris No 2 Continuum Observationssupporting

confidence: 82%

Section: Introductionmentioning

confidence: 99%

NO₂ air afterglow and O and NO densities from Odin‐OSIRIS night and ACE‐FTS sunset observations in the Antarctic MLT region

et al. 2010

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“…The FeO * component must be removed from the total residual continuum to isolate any previously unidentified features. Least squares combinations of the model mesospheric FeO * spectral profile (Gattinger et al, 2011b) and the model NiO * spectral profile (Gattinger et al, 2011a), along with the NO * 2 spectral profile (Becker et al, 1972;Gattinger et al, 2009) known to be present in varying amounts (McDade et al, 1986), are applied to the GLO-1 residual continuum in Fig. 4.…”

Section: Night Airglow Continuum Observations With the Glo-1 Spectrogmentioning

confidence: 99%

“…However, new emission features are still being identified, an example being the FeO "orange" bands that arise from the reaction between atomic iron of meteoric origin with terrestrial ozone . Known emission features continue to be investigated and their spectral signatures more accurately determined; such as the chemiluminescent emission of NO * 2 that is produced in the NO + O reaction (Becker et al, 1972;Gattinger et al, 2010). Extending these ongoing observations, it is expected that a chemiluminescent emission from NiO * , which also arises from the reaction of atomic nickel of meteoric origin (McNeil et al, 1998) with atmospheric ozone, should be present in the airglow spectrum, albeit very faint.…”

Section: Introductionmentioning

confidence: 96%

The observation of chemiluminescent NiO* emissions in the laboratory and in the night airglow

et al. 2011

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Abstract. The recent finding of an orange spectral feature in OSIRIS/Odin spectra of the night airglow near 87 km has raised interest in the origin of the emission. The feature was positively identified as the chemiluminescent FeO * emission where the iron is of meteoric origin. Since the meteorite source of atomic metals in the mesosphere contains both iron and nickel, with Ni being typically 6 % of Fe, it is expected that faint emissions involving Ni should also be present in the night airglow. The present study summarizes the laboratory observations of chemiluminescent NiO * emissions and includes a search for the NiO * signature in the night airglow. A very faint previously unidentified "continuum" extending longwave of 440 nm has been detected in the night airglow spectra obtained with two space-borne limb viewing instruments. Through a comparison with laboratory spectra this continuum is identified as arising from the NiO * emission. The altitude profile of the new airglow emission has also been measured. The similarity of the altitude profiles of the FeO * and NiO * emissions also suggests the emission is NiO as both can originate from reaction of the metal atoms with mesospheric ozone. The observed NiO * to FeO * ratio exhibits considerable variability; possible causes of this observed variation are briefly discussed.

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“…The first term within braces on the right of the equation (7)is dominant when [MI is low and the second term is dominant when [MI is high. Published information (Becker et al 1972)enables the values of k,, k3/k2 and k,/A a t 296 K a t any chosen wavelength to be found.…”

Section: Drbatesmentioning

confidence: 99%

Cause of terrestrial nightglow continuum

Bates

1993

Proc. R. Soc. Lond. A

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Since the nightglow’s green continuum was discovered over 40 years ago the theory that it arises from the NO 2 air afterglow has been generally accepted so that its intensity is regarded as a useful measure of the abundance of nitric oxide in the lower thermosphere. This theory is shown to be untenable. Observational evidence points unambiguously to a novel source: metastable oxygen molecules colliding with ambient gas molecules and thereby forming complexes that dissociate by allowed radiative transitions.

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Mechanism of the air afterglow NO+O→NO2+hv

Cited by 19 publications

References 38 publications

NO₂ air afterglow and O and NO densities from Odin‐OSIRIS night and ACE‐FTS sunset observations in the Antarctic MLT region

NO₂ air afterglow and O and NO densities from Odin‐OSIRIS night and ACE‐FTS sunset observations in the Antarctic MLT region

The observation of chemiluminescent NiO* emissions in the laboratory and in the night airglow

Cause of terrestrial nightglow continuum

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Mechanism of the air afterglow NO+O→NO2+hv

Cited by 19 publications

References 38 publications

NO2 air afterglow and O and NO densities from Odin‐OSIRIS night and ACE‐FTS sunset observations in the Antarctic MLT region

NO2 air afterglow and O and NO densities from Odin‐OSIRIS night and ACE‐FTS sunset observations in the Antarctic MLT region

The observation of chemiluminescent NiO* emissions in the laboratory and in the night airglow

Cause of terrestrial nightglow continuum

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Product

Resources

About

NO₂ air afterglow and O and NO densities from Odin‐OSIRIS night and ACE‐FTS sunset observations in the Antarctic MLT region

NO₂ air afterglow and O and NO densities from Odin‐OSIRIS night and ACE‐FTS sunset observations in the Antarctic MLT region