Rate constant for the infrared emission of the NO(C2Π → A2Σ+) transition

Groth, W.; Kley, D.; Schurath, U.

doi:10.1016/0022-4073(71)90109-9

Cited by 54 publications

(34 citation statements)

References 11 publications

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“…Such spectra easily compare with the laboratory spectrum of the N( 4 S) + O( 3 P) recombination (Groth et al, 1971), or with a limb NO spectrum from Gé rard et al (2008). The identification is therefore positive as an NO emission, and thus we can safely assume that this feature is the one contaminating the stellar spectrum when the slit is removed and spectroscopic information is lost.…”

Section: Observation Of the No Emissionmentioning

confidence: 96%

NO emissions as observed by SPICAV during stellar occultations

Royer

Montmessin

Bertaux

2010

Planetary and Space Science

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Section: Observation Of the No Emissionmentioning

confidence: 96%

NO emissions as observed by SPICAV during stellar occultations

Royer

Montmessin

Bertaux

2010

Planetary and Space Science

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“…ls Our estimate made on the basis of peak intensity on the 15 bands from a low pressure recombination spectrum 19 indicates a slight linear dependence of the electronic transition moment on v". However, those data are insufficient to establish the variation of R,(v") with reasonable accuracy and in the above calculation we have assumed R.(v") to be independent of v".…”

Section: Resultsmentioning

confidence: 99%

Predissociation and its inverse, using resonance absorption NO(C 2Π) ⇄ N+O

Mandelman

Carrington

Young

1973

The Journal of Chemical Physics

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Radiative recombination of N+O has been investigated by using this radiation as a highly specific light source for dissociation of NO. This direct proof of predissociation of NO(C 2Π) supports previous indirect evidence. Measurements of the rate of N2 production in the photodissociation lead to a rate coefficient for the process N+O ⇄ NO(C 2Π, v′ = 0) → NO(X 2Π, v″ = 0) + hν, kδ0,0 = (2.9 ± 0.5) × 10−18 cm3 sec−1 at 300°K. The total rate coefficient summed over v″ is (1.5 ± 0.4) × 10−17 cm3 sec.−1 When N and O concentrations are measured by titration, the recombination emission can be used as an absolute intensity standard (±20%) at 1900 Å.

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“…In turn, this implies that, in the nightglow, the emission rates for the C(0) 3 A(0) and A(0) 3 X(vЉ) transitions are the same, and that the ratio of the emission rate for C(0) 3 A(0) to the sum of the emission rates for C(0) 3 X(vЉ) and C(0) 3 A(0) is constant. Estimates of this branching ratio based on laboratory, theoretical, and observational investigations lie in the range 0.21Ϫ0.41 (9,(20)(21)(22)(23)(24)(25)(26). Some of these studies were adversely affected by contamination or by uncertain calibrations, so a consensus on a precise value has not yet been reached.…”

Section: Nitric Oxide Deactivation Branching Ratiomentioning

confidence: 99%

“…The C(0) 3 A(0) band comprises P, Q, and R main branches, with the lines of the stronger Q branch building up at Ϸ1.224 m and those of the P and R branches spreading on either side toward longer and shorter wavelengths, respectively (30). At moderate to low spectral resolutions, however, the band spectrum looks more like a single line at the position of the Q branch (20,31,32). …”

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confidence: 99%

The near-infrared nitric oxide nightglow in the upper atmosphere of Venus

Muñoz

Mills

Piccioni

et al. 2009

Proc. Natl. Acad. Sci. U.S.A.

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The v ‫؍‬ 0 progressions of the C 3 X and A 3 X band systems of nitric oxide dominate the middle-UV spectrum of the night-time upper atmospheres of the Earth, Mars, and Venus. The C(0) 3 A(0)؉h radiative transition at 1.224 m, the only channel effectively populating the A(0) level, must therefore occur also. There have been, however, no reported detections of the C(0) 3 A(0) band in the atmospheres of these or any other planets. We analyzed all available near-infrared limb observations of the darkside atmosphere of Venus by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument on the Venus Express spacecraft and found 2 unambiguous detections of this band at equatorial latitudes that seem to be associated with episodic events of highly enhanced nightglow emission. The discovery of the C(0) 3 A(0) band means observations in the 1.2-1.3 m region, which also contains the a(0) 3 X(0) emission band of molecular oxygen, can provide a wealth of information on the high-altitude chemistry and dynamics of the Venusian atmosphere.T he luminescence that results from exothermic chemical reactions between the constituents of a planetary atmosphere is customarily termed the night airglow or, simply, the nightglow (1). Although possibly present all day long, it appears most distinctly at night when the other processes of atomic and molecular excitation that depend directly on the action of the Sun are not at play and the diffuse radiation of solar light is at its minimum. The nightglow may originate from various, possibly minor, atmospheric constituents and provides insight into the chemistry, composition, temperature and energy balance of the atmosphere of a planet.The C 2 ⌸ 3 X 2 ⌸ and A 2 ⌺ ϩ 3 X 2 ⌸ band systems of nitric oxide (often referred to as the ␦ and ␥ bands, respectively) have long been known in the upper-atmospheric nightglow of the Earth (2, 3) and Venus (4, 5). More recently, they have also been reported in the atmosphere of Mars (6). A common structure, caused by the vЈ ϭ 0 progression of the aforementioned systems, characterizes the night-time middle-UV spectrum of all 3 planets. Separately and in combination with other nightglow emissions, observations of the nitric oxide nightglow have been used to infer details of the odd-nitrogen chemistry and dynamics in the emitting atmospheres.In the dayglow, resonance scattering of solar photons from ground-state nitric oxide gives rise to additional A 3 X (vЈ Ն 0) bands that have been observed on the sunlit side of the Earth (7) but that remain undetected in the atmospheres of Mars and Venus. On Mars, and expectedly also on Venus, the emission of the a 3 ⌸ 3 X 1 ⌺ system of carbon monoxide is likely to mask the nitric oxide A 3 X dayglow (8). The fluorescence efficiency of the C state is low for v ϭ 0 and negligible for vϾ0, presumably due to rapid predissociation (9-12). Day-time observations of the terrestrial atmosphere have found weak C 3 X (vЈ ϭ 0) bands, which have been attributed to resonance scattering (13-15), although there are significa...

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Rate constant for the infrared emission of the NO(C2Π → A2Σ+) transition

Cited by 54 publications

References 11 publications

NO emissions as observed by SPICAV during stellar occultations

NO emissions as observed by SPICAV during stellar occultations

Predissociation and its inverse, using resonance absorption NO(C 2Π) ⇄ N+O

The near-infrared nitric oxide nightglow in the upper atmosphere of Venus

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