Association of atomic oxygen and airglow excitation mechanisms

Wraight, P.C.

doi:10.1016/0032-0633(82)90003-4

Cited by 93 publications

(39 citation statements)

References 42 publications

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“…This suggestion was based on calculations of the efficiency of production of various states ofO 2 by Wraight (1982) and Smith (1984) that showed that the 5//g state is produced with about a 66~o efficiency. Bates (1988b) proposed that the fraction be reduced to 50~o to account for the smaller potential well depth of the 5I-Ig state, about 0.14 eV as computed by Partridge et aI.…”

Section: No Nightglowmentioning

confidence: 99%

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Structure, luminosity, and dynamics of the Venus thermosphere

Fox

Bougher

1991

Space Sci Rev

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We review here observations and models related to the chemical and thermal structures, airglow and auroral emissions and dynamics of the Venus thermosphere, and compare empirical models of the neutral densities based in large part on in situ measurements obtained by the Pioneer Venus spacecraft.Observations of the intensities of emissions are important as a diagnostic tool for understanding the chemical and physical processes taking place in the Venus thermosphere. Measurements, ground-based and from rockets, satellites, and spacecraft, and model predictions of atomic, molecular and ionic emissions, are presented and the most important sources are elucidated. Coronas of hot hydrogen and hot oxygen have been observed to surround the terrestrial planets. We discuss the observations of and production mechanisms for the extended exospheres and models for the escape of lighter species from the atmosphere. Over the last decade and a half, models have attempted to explain the unexpectedly cold temperatures in the Venus thermosphere; recently considerable progress has been made, although some controversies remain. We review the history of these models and discuss the heating and cooling mechanisms that are presently considered to be the most important in determining the thermal structure. Finally, we discuss major aspects of the circulation and dynamics of the thermosphere: the sub-solar to anti-solar circulation, superrotation, and turbulent processes.

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Section: No Nightglowmentioning

confidence: 99%

“…Moreover, Krasnopol'sky's 1981 analysis preceded the calculations of Wraight (1982) and Smith (1984) and was based on a statistical distribution of states of 0 2 formed in the three-body recombination.…”

Section: No Nightglowmentioning

confidence: 99%

Structure, luminosity, and dynamics of the Venus thermosphere

Fox

Bougher

1991

Space Sci Rev

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“…10 At night, O 2 (b 1 ⌺ g ϩ ) is generated from oxygen atom three-body recombination, and potentially a large range of vibrational levels in the b 1 ⌺ g ϩ state is produced. [19][20][21] That emission from these vibrationally-excited O 2 (b 1 ⌺ g ϩ ) levels has, until recently, only been reported in aurora 10,11 and not in the nightglow suggests that removal of vibrationallyexcited levels is very rapid compared to vϭ0. This vibrational-level-dependent removal is well established for the vϭ1 level from laboratory investigations, where, for O 2 as collider, there is some six orders-of-magnitude difference in removal rate coefficient for vϭ0 ͑Ref.…”

Section: Introductionmentioning

confidence: 97%

Collisional removal of O2(b 1Σg+,v=1,2) by O2, N2, and CO2

Bloemink

Copeland

Slanger

1998

The Journal of Chemical Physics

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A state-specific two-laser technique is used to investigate the collisional removal of O 2 molecules in the b 1 ⌺ g ϩ (vϭ1,2) levels, where we directly excite O 2 and then probe the populations by resonance-enhanced multiphoton ionization. We find general agreement with earlier 300 K values for vϭ1 removal by O 2 , and show that vϭ2 removal is slower by a factor of 5.6Ϯ0.6 than vϭ1 removal. Only upper limits are obtained for N 2 as a collider. For removal of vϭ1 in the atmosphere, N 2 is unimportant compared to O 2 , but it might be competitive for vϭ2. For CO 2 as a collider, addressing O 2 (b 1 ⌺ g ϩ ) removal in the atmospheres of Mars and Venus, the removal rate coefficients of the vibrationally-excited levels are similar to that for vϭ0. The significance of the large difference in the vϭ1 and vϭ2 rate coefficients for O 2 collisions will be discussed as it relates to the modeling of recent earth nightglow observations.

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“…In view of the result of Ali et al [1986], and of calculations that also show that the expected O 2 ( a 1 Δ g ) yield from process is only several percent [ Bates , 1988; Wraight , 1982], the modeling community began considering process , as an additional source of atmospheric O 2 ( a 1 Δ g ) [ Howell et al , 1990; Kita et al , 1992; López‐González et al , 1992; McDade et al , 1987]. Several studies have indicated that, in addition to processes (1a) (2, 3), other sources of O 2 ( a 1 Δ g ) must be considered in order to explain the observed emission rates [ Howell et al , 1990; Kita et al , 1992; McDade et al , 1987].…”

Section: Introductionmentioning

confidence: 99%

“…Theoretical work has initially suggested that the weakly bound 5 Π g state is the principal precursor state [ Smith , 1984; Wraight , 1982]. However, Bates [1988] argues, on the basis of more recent theoretical curves for the relevant states, that the A 3 Σ u + , A ′ 3 Δ u , and c 1 Σ u − states taken together may also be important as precursors.…”

Section: Introductionmentioning

confidence: 99%

Studies on the production of O₂(a¹Δ_g, υ = 0) and O₂(b¹Σ_g⁺, υ = 0) from collisional removal of O₂(A³Σ_u⁺, υ′ = 6–10)

et al. 2007

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in synthetic air are nearly equal to those measured in pure O 2 , suggesting that N 2 collider does not significantly affect the relaxation pathways leading to the production of the two metastable species. However, at short experimental times the buildup of the O 2 (a 1 D g , u = 0) population is considerably slower in synthetic air than in O 2 . Introduction[2] In the upper atmospheres of the Earth and Venus oxygen atoms recombine via a three-body process to produce a variety of excited species of molecular oxygen. As a result, emissions from the five low-lying excited electronic states (A Atmospheric bands, which are among the strongest components of the nightglow. The detailed information on the yields of these two species from three-body recombination of oxygen atoms is important for modeling of the observed relative and absolute nightglow emission intensities. In particular, production pathways and the effects of the collisional environment (i.e., type and pressure of the collider) on these yields must be established.[3] An obvious mechanism for production of O 2 (a 1In the atmosphere, M is primarily O 2 /N 2 , although in principle the third body can be a third oxygen atom, as initially proposed by Chapman

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Association of atomic oxygen and airglow excitation mechanisms

Cited by 93 publications

References 42 publications

Structure, luminosity, and dynamics of the Venus thermosphere

Structure, luminosity, and dynamics of the Venus thermosphere

Collisional removal of O2(b 1Σg+,v=1,2) by O2, N2, and CO2

Studies on the production of O₂(a¹Δ_g, υ = 0) and O₂(b¹Σ_g⁺, υ = 0) from collisional removal of O₂(A³Σ_u⁺, υ′ = 6–10)

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Association of atomic oxygen and airglow excitation mechanisms

Cited by 93 publications

References 42 publications

Structure, luminosity, and dynamics of the Venus thermosphere

Structure, luminosity, and dynamics of the Venus thermosphere

Collisional removal of O2(b 1Σg+,v=1,2) by O2, N2, and CO2

Studies on the production of O2(a1Δg, υ = 0) and O2(b1Σg+, υ = 0) from collisional removal of O2(A3Σu+, υ′ = 6–10)

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Studies on the production of O₂(a¹Δ_g, υ = 0) and O₂(b¹Σ_g⁺, υ = 0) from collisional removal of O₂(A³Σ_u⁺, υ′ = 6–10)