Morning and evening behavior of the F region green line emission: Evidence concerning the sources of O(¹S)

Kopp, J.; Frederick, John E.; Rusch, D. W.; Victor, G. A.

doi:10.1029/ja082i029p04715

Cited by 33 publications

(8 citation statements)

References 7 publications

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“…However, the N + density is so small that this reaction accounts for less than one percent of the emission. Frederick et al (1976); Kopp et al (1977) propose a similar kind of reactions: O ) + O( 1 S) is spin-forbidden. However many cases of spin-forbidden reactions are known to occur with good efficiency because of strong spin-orbit couplings (Scott et al 1998).…”

Section: A3 the O 2 + + N Processmentioning

confidence: 97%

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Modelling the Venusian airglow

Gronoff¹,

Lilensten²,

Simon

et al. 2008

A&A

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Context. Modelling of the Venusian ionosphere fluorescence is required, to analyse data being collected by the SPICAV instrument onboard Venus Express. Aims. We present the modelling of the production of excited states of O, CO and N 2 , which enables the computation of nightglow emissions. In the dayside, we compute several emissions, taking advantage of the small influence of resonant scattering for forbidden transitions. Methods. We compute photoionisation and photodissociation mechanisms, and the photoelectron production. We compute electron impact excitation and ionisation, through a multi-stream stationary kinetic transport code. Finally, we compute the ion recombination using a stationary chemical model. Results. We predict altitude density profiles for O( 1 S) and O( 1 D) states, and emissions corresponding to their different transitions. They are found to agree with observations. In the nightside, we discuss the different O( 1 S) excitation mechanisms as a source of green line emission. We calculate production intensities of the O( 3 S) and O( 5 S) states. For CO, we compute the Cameron bands and the Fourth Positive bands emissions. For N 2 , we compute the LBH, first and Second Positive bands. All values are compared successfully to experiments when data are available. Conclusions. For the first time, a comprehensive model is proposed to compute dayglow and nightglow emissions of the Venusian upper atmosphere. It relies on previous works with noticeable improvements, both on the transport side and on the chemical side. In the near future, a radiative-transfer model will be used to compute optically-thick lines in the dayglow, and a fluid model will be added to compute ion densities.

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Section: A3 the O 2 + + N Processmentioning

confidence: 97%

“…Back in the 1970s, Frederick et al (1976); Kopp et al (1977) proposed a new reaction in the Earth's thermosphere:…”

mentioning

confidence: 99%

Modelling the Venusian airglow

Gronoff¹,

Lilensten²,

Simon

et al. 2008

A&A

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“…The predicted 6300-A intensity (Figure 3b In a more recent laboratory experiment, Zipf [1980] determined that the yield of O(•S) in the dissociative recombination of O2 + is dependent upon the degree of vibrational excitation of the O2 + ion, with the yield for v = 0-3 being substantially lower (2%) than for v > 3 (10%). Subsequently, Bates and Zipf [1980] proposed that the yield may also be dependent upon electron temperature in order to reconcile the 9% value inferred from a satellite dayglow analysis [Kopp et al, 1977] with the expected efficiency of vibrational quenching by atomic oxygen. However, the most recent laboratory results (E. C. Zipf, private communication, 1983) show that (1) the higher yield inferred from the earlier experiments [Zipf, 1970[Zipf, , 1980 (Table 7), which are in agreement in spite of the fact that the rocket only views the emission originating above 200 km in the cleft.…”

Section: -T' Emissionmentioning

confidence: 99%

An analysis of the spatial distribution of dayside cleft optical emissions

Link¹,

McConnell²,

Shepherd³

1983

J. Geophys. Res.

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An analysis of measurements of the 4278-A, 5200-A, 5577-A, and 6300-A emissions obtained from a rocket launch through the postnoon dayside cleft into the polar cap ionosphere is reported. The 4278-A and 5577-• emissions show a clearly defined decrease in intensity at the poleward.edge of the dayside particle precipitation, while the 5200-A emission extends well into the polar cap with only a slight decrease in intensity. The 6300-A emission displays a behavior intermediate between these extremes. The optical data are analysed by using a dynamical model of dayside cleft auroral processes incorporating transport by ion and neutral winds. It is concluded that neutral winds are responsible for modifying the spatial distribution of the 5200-A and 6300-A emission, while the ion drift component is negligible. In addition, it is found that (1) 80% of the 4278-A emission intensity is due to resonance fluorescence in the sunlit cleft ionosphere, (2) the reaction O2(c•Y',., -) + O• O 2 + O(•S) is consistent with the 5577-• data if the yield of O(•S) from the dissociative recombination of 02 + is about 2%, and (3) the rate of the reaction N2 + + O• NO + + N is apparently higher in the ionosphere than indicated by the laboratory measurements. examination of both ion drift and neutral wind effects and is based on the study of Link [1982]. Preliminary results from this study have been presented by Link et al. [1976, 1978]. Recently, G•rard and Roble [1982] have presented an independent analysis of the AMF-VB-41 5200-J• data, based on a neutral wind transport model. More recently, Link [1983] has discussed the implications of the spatial distribution of the 5200-J• emission for the mechanisms of O(XD) production. CLEFT CAMPAIGN MEASUREMENTSThe following section presents optical and other supporting measurements obtained from the Black Brant AMF-VB-41

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“…In a recent paper, Zipf[1979b] The discrepancy between the large O(IS) quantum yield e(IS) for reaction (1) obtained by Zipf[1970] in a laboratory plasma spectroscopy study (10%) and the values of 8.0 and 9.9% derived from an analysis of Atmosphere Explorer (AE) airglow observations by Frederick et al [1976] and Kopp et al [1977], respectively, on the one hand, and the much lower values obtained in a sounding rocket study of the 3,5577-,3, nightglow (3% [Hays and Sharp, 1973]), from a ground-based interferometric study of the equatorial airglow (4% [Hernandez, 1971]), and from the Precede experiment (2-3% [Zipf, 1979]) on the other hand, was attributed to a variation of the O(IS) specific dissociative recombination coefficient with the vibrational quantum number of the recombining 02 + ion. The agreement between the laboratory value for E(IS) and the AE observational results was taken then as evidence that most 02 + ions in the sunlit F region are vibrationally excited and that they remain vibrationally hot throughout their effective atmospheric lifetimes.…”

Section: Introductionmentioning

confidence: 98%

A laboratory study on the dissociative recombination of vibrationally excited O₂⁺ ions

Zipf¹

1980

J. Geophys. Res.

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The production of metastable O(¹S) atoms by the dissociative recombination of O2+ ions has been studied in a laboratory plasma spectroscopy experiment. The specific dissociative recombination coefficient for O(1S) formation has a value of 2.1 × 10−8 cm3 s−1, corresponding to an O(¹S) quantum yield of 10% at an apparent temperature of 296°K, in agreement with the earlier but less comprehensive measurements of Zipf [1970]. By using a variety of gas mixtures in order to modify the vibrational population of the O2+ ions and laser‐induced photofluorescence techniques it was found that the laboratory O2+ plasmas are vibrationally excited and that O2+ ions in the υ′=4–12 vibrational levels are the chief source of the observed O(1S) atoms. The specific O(1S) dissociative recombination coefficient for O2+(2πg) ions in the lowest vibrational levels (υ′ ≤3) is much smaller (4.2 × 10−9 cm3 s−1). The implications of the quantum yield of 9.9% derived from Atmosphere Explorer data are discussed in the light of these findings. Preliminary electron‐heating experiments indicate that the specific O(¹S) recombination coefficient decreases with increasing electron temperature.

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Morning and evening behavior of the F region green line emission: Evidence concerning the sources of O(¹S)

Cited by 33 publications

References 7 publications

Modelling the Venusian airglow

Modelling the Venusian airglow

An analysis of the spatial distribution of dayside cleft optical emissions

A laboratory study on the dissociative recombination of vibrationally excited O₂⁺ ions

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Morning and evening behavior of the F region green line emission: Evidence concerning the sources of O(¹S)

Cited by 33 publications

References 7 publications

Modelling the Venusian airglow

Modelling the Venusian airglow

An analysis of the spatial distribution of dayside cleft optical emissions

A laboratory study on the dissociative recombination of vibrationally excited O2+ ions

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Product

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A laboratory study on the dissociative recombination of vibrationally excited O₂⁺ ions