OH(<i>ν,N</i>) column densities from high‐resolution Earthlimb spectra

Dodd, James A.; Blumberg, W. A. M.; Lipson, Stephen J.; Lowell, J. R.; Armstrong, Peter S.; Smith, Donald R.; Nadile, R. M.; Wheeler, N. B.; Huppi, E. R.

doi:10.1029/93gl00091

Cited by 17 publications

(13 citation statements)

References 10 publications

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“…The accurate determination of tangent heights is crucial in the case of OH emission at the mesopause, since the radiance occurs over such a small altitude range. As discussed previously Dodd et al, 1993a], the observed OH(v,N) line intensities are very sensitive to the interferometer viewing angle. At the 100-km tangent height a change in pitch angle of 10 mrad (0.6 ø) results in a tangent height change of 15 km, providing a very sensitive means of discriminating against the possible effects of shuttle-induced radiance.…”

Section: Tangent Height Determinationmentioning

confidence: 65%

Analysis of hydroxyl earthlimb airglow emissions: Kinetic model for state‐to‐state dynamics of OH (υ,N)

Dodd¹,

Lipson²,

Lowell³

et al. 1994

J. Geophys. Res.

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Detailed spectroscopic analysis of hydroxyl fundamental vibration‐rotation and pure rotation emission lines has yielded OH(υ,N) absolute column densities for nighttime earthlimb spectra in the 20 to 110‐km tangent height region. High‐resolution spectra were obtained in the Cryogenic Infrared Radiance Instrumentation for Shuttle (CIRRIS 1A) experiment. Rotationally thermalized populations in υ = 1–9 have been derived from the fundamental bands between 2000 and 4000 cm−1. Highly rotationally excited populations with N ≤ 33 ( ≤ 2.3 eV rotational energy) have been inferred from the pure rotation spectra between 400 and 1000 cm−1. These emissions originate in the airglow region near 85–90 km altitude. Spectral fits of the pure rotation lines imply equal populations in the spinrotation states F1 and F2 but a ratio Π(A′):Π(A″) = 1.8±0.3 for the Λ‐doublet populations. A forward predicting, first‐principles kinetic model has been developed for the resultant OH(υ,N) limb column densities. The kinetic model incorporates a necessary and sufficient number of processes known to generate and quench OH(υ,N) in the mesopause region and includes recently calculated vibration‐rotation Einstein coefficients for the high‐N levels. The model reproduces both the thermal and the highly rotationally excited OH(υ,N) column densities. The tangent height dependence of the rotationally excited OH(υ,N) column densities is consistent with two possible formation mechanisms: (1) transfer of vibrational to rotational energy induced by collisions with O atoms or (2) direct chemical production via H + O3 → OH(υ,N) + O2.

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Section: Tangent Height Determinationmentioning

confidence: 65%

Analysis of hydroxyl earthlimb airglow emissions: Kinetic model for state‐to‐state dynamics of OH (υ,N)

Dodd¹,

Lipson²,

Lowell³

et al. 1994

J. Geophys. Res.

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“…For the case of OH, a 200 K rotational distribution only approximates the actual population distribution in the lower rotational levels [ Cosby and Slanger , 2006]; however, this approximation is sufficiently accurate for confident identification of the OH lines. As noted by Pendleton et al [1989] and by Dodd et al [1993], the population distribution in higher rotational levels of OH ( J ′ ≥ 7.5) is much hotter. We follow the population distributions given by Cosby and Slanger [2006] to model these high levels for the identifications.…”

Section: Identification Proceduresmentioning

confidence: 77%

High‐resolution terrestrial nightglow emission line atlas from UVES/VLT: Positions, intensities, and identifications for 2808 lines at 314–1043 nm

et al. 2006

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[1] The atlas of terrestrial nightglow emission lines from spectra of the night sky obtained from the Ultraviolet and Visual Echelle Spectrograph (UVES) on the 8.2-m UT2 telescope at the Very Large Telescope (VLT), European Southern Observatory, Cerro Paranal, Chile, consists of 2808 line positions, line widths, and intensities over the 314-1043 nm spectral range (Hanuschik, 2003). These lines have been absolute intensity calibrated and measured at a spectral resolution (l/Dl) of $43,000-45,000. Presented here are spectroscopic identifications for 98% of the lines in the atlas, made primarily through comparisons with synthetic spectra of prominent OH and O 2 nightglow emission systems. The ability to simulate these systems successfully has shown that there are many additional lines that could be added to the atlas. We believe that all the O 2 and OH lines in the measured region can now be successfully modeled with an accuracy better than the instrumental spectral resolution.

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“…cm -1 region for a tangent height of 85 km, the spectrum obtained as the average of three spectra with similar tangent heights and emission intensities. Spectra such as that shown in Figure 1 were fit using methods described in a previous publication [Dodd et al, 1993]. Observed radiance was found to be closely reproduced at all tangent heights by including six molecular bands: the 03 vl+v 3 (band origin 2111 cm 'l) and vl+v:+v3-v: (2084 cm 'l) combination bands, the OH 9-8 band (2236 cm-1), and the 1-0 bands of nClaO (2143 cm-1), 13ClaO (2096 cm-1), and nC180 (2092 cm'l).…”

Section: Subtraction Of Modeled 03 Oh and 12c160 (Main Isotope) Radmentioning

confidence: 99%

“…We have previously reported a preliminary analysis of high-altitude earthlimb emission spectra from the CIRRIS 1A experiment in the 4.7 •m region [Dodd et al, 1993].…”

Section: Introductionmentioning

confidence: 99%

CIRRIS 1A observation of ¹³C¹⁶O and ¹²C¹⁸O fundamental band radiance in the upper atmosphere

Dodd¹,

Winick²,

Blumberg³

et al. 1993

Geophysical Research Letters

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Fundamental band emission from the ν=1 levels of isotopically substituted 13C16O and 12C18O has been observed for the first time in the earth's atmosphere. High‐resolution earthlimb spectra were obtained in the Cryogenic Infrared Radiance Instrumentation for Shuttle (CIRRIS 1A) experiment under both nighttime and daytime conditions. Spectral data between 70 and 150 km tangent height were analyzed in the 4.7 µm wavelength region, providing absolute 12C16O, 13C16O, and 12C18O column radiances. The minor isotope column radiances are up to 30 times more intense than predicted, based solely on the natural isotopic abundances of 13C and 18O. The derived line‐of‐sight radiances were accurately modeled using the Phillips Laboratory Atmospheric Radiance Code, and provide a strong test of radiative transport and excitation algorithms, as well as model climatologies.

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OH(ν,N) column densities from high‐resolution Earthlimb spectra

Cited by 17 publications

References 10 publications

Analysis of hydroxyl earthlimb airglow emissions: Kinetic model for state‐to‐state dynamics of OH (υ,N)

Analysis of hydroxyl earthlimb airglow emissions: Kinetic model for state‐to‐state dynamics of OH (υ,N)

High‐resolution terrestrial nightglow emission line atlas from UVES/VLT: Positions, intensities, and identifications for 2808 lines at 314–1043 nm

CIRRIS 1A observation of ¹³C¹⁶O and ¹²C¹⁸O fundamental band radiance in the upper atmosphere

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OH(ν,N) column densities from high‐resolution Earthlimb spectra

Cited by 17 publications

References 10 publications

Analysis of hydroxyl earthlimb airglow emissions: Kinetic model for state‐to‐state dynamics of OH (υ,N)

Analysis of hydroxyl earthlimb airglow emissions: Kinetic model for state‐to‐state dynamics of OH (υ,N)

High‐resolution terrestrial nightglow emission line atlas from UVES/VLT: Positions, intensities, and identifications for 2808 lines at 314–1043 nm

CIRRIS 1A observation of 13C16O and 12C18O fundamental band radiance in the upper atmosphere

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CIRRIS 1A observation of ¹³C¹⁶O and ¹²C¹⁸O fundamental band radiance in the upper atmosphere