Ratio of the O2(¹Δg- ³Σg−) (0, 0) (0, 1) transitions

Haslett, J. C.; Fehsenfeld, F. C.

doi:10.1029/ja074i007p01878

Cited by 9 publications

(3 citation statements)

References 4 publications

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“…There have been a few subsequent estimates of the ratio, that have come either from laboratory experiments, e.g., A 00 /A 01 = 46.0 ± 0.7 [ Findlay , 1969], 49.5 ± 4 [ Becker et al , 1971], 80 ± 20 [ Haslett and Fehsenfeld , 1969], and 55 ± 10 [ Thomas and Thrush , 1977]; or from airglow observations, some times in combination with photochemical modeling, e.g., A 00 /A 01 = 52 ± 25 [ Winick et al , 1985], and 80 ± 15 [ Pick et al , 1971]. More recently, Kassi et al [2005] have determined the line strengths of a few lines belonging to the strong Q branch in a high‐resolution absorption spectrum experiment.…”

Section: Oxygen Band Ratiomentioning

confidence: 99%

Near‐IR oxygen nightglow observed by VIRTIS in the Venus upper atmosphere

Piccioni¹,

Zasova²,

Migliorini³

et al. 2009

J. Geophys. Res.

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[1] We present observations of both the (0-0) and (0-1) bands at 1.27 and 1.58 mm of the O 2 (a 1 D g À X 3 S g À ) nightglow made with the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument aboard Venus Express. The observations were conducted in both nadir and limb viewing modes, the latter constituting the first systematic investigation into the vertical distribution of the volume emission rate of the infrared oxygen nightglow in Venus' upper atmosphere. Limb measurements from 42 orbits covering the latitude range 7°S to 77°N are analyzed. The peak altitude of the volume emission rate occurs typically between 95 and 100 km, with a mean of 97.4 ± 2.5 km. The vertical profile is broader near the equator, with a full width at half maximum of 11 km, a factor 2 larger than at middle latitudes. A double peak is frequently observed, with the lower and upper peaks occurring near 96-98 km and 103-105 km, respectively. On average, the nightglow appears brightest in the vicinity of the antisolar point. This conclusion is consistent with past ground-based observations and nadir measurements by VIRTIS. We mapped the global mean O 2 nightglow intensity from VIRTIS data collected during 880 orbits. Patchy features of the nightglow intensity observed in nadir view are correlated with the thermal brightness at 4.23-4.28 mm. The observed positive correlation is consistent with downwelling (upwelling) of oxygen atoms accompanying compressional heating (expansion cooling) or with modulation by gravity waves. Finally, from simultaneous measurements of the 1.27 and 1.58 mm bands, we have estimated the ratio of the transition probabilities A 00 /A 01 to be 63 ± 8.

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Section: Oxygen Band Ratiomentioning

confidence: 99%

Near‐IR oxygen nightglow observed by VIRTIS in the Venus upper atmosphere

Piccioni¹,

Zasova²,

Migliorini³

et al. 2009

J. Geophys. Res.

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“…The origin of this structure is still poorly understood, even though it seems to have a strict correlation with dynamics. In the terrestrial case, the (0-1) O 2 band at 1.58 lm is 40-146 times less intense than the (0-0) band, as determined from ground-based airglow observations (Pick et al, 1971;Winick et al, 1985), laboratory (Findlay, 1969;Noxon, 1967;Haslett and Fehsenfeld, 1969;Becker et al, 1971), or from models (Krupenie, 1972;Pick et al, 1971). However, it was the first to be observed from ground at twilight (Vallance Jones and Harrison, 1958).…”

Section: Introductionmentioning

confidence: 82%

Comparative analysis of airglow emissions in terrestrial planets, observed with VIRTIS-M instruments on board Rosetta and Venus Express

Migliorini

Piccioni

Capaccioni

et al. 2013

Icarus

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a b s t r a c tAirglow emissions are optimal processes to investigate the chemistry and dynamics in planetary atmospheres. In this study, we focus on the O 2 and OH airglow emissions in Venus, Earth, and Mars atmospheres, which are controlled by chemical reactions common to the three planets. By studying these phenomena on Venus, Earth, and Mars using similar instruments, we are able to derive information about their photochemistry and the physical conditions of the atmospheres, but also to constrain the dynamics responsible for transport of atomic oxygen, ozone and other minor species.After a review of the nightglow emissions observed in the Venus atmosphere, we analyze the O 2 and OH airglow emissions in the Earth's atmosphere observed during the 3 swing-bys of our planet by the Rosetta spacecraft.We also report the detection of the O 2 nightglow emission in the Mars atmosphere, observed in February 2007 during the Rosetta fly-by of the planet. The airglow characteristics are in agreement with the measurements obtained from sensors on board Mars Express.

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“…The transition probability is given as A00=2.6x 10-sec-1 for the (0,0) band (BADGER et al, 1965), and A01=3.5x10-6sec-1 for the (0,1) band (HASLETT and FEHSENFELD, 1969). Thus the total transition probability for v'=0 of the 149 state if A=Aoi-Aoo.…”

Section: Discussionmentioning

confidence: 99%