Calculated OH A2Σ+−X2Π (0,0) band rotational emission rate factors for solar resonance fluorescence

Stevens, M. H.; Conway, Robert R.

doi:10.1029/1998jd100073

Cited by 13 publications

(31 citation statements)

References 31 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Precise laboratory measurements are required to reduce this large uncertainty. Stevens and Conway [10] estimate a root-sum-square error of 7% for the OH 0-0 band g-factors, and Crosley and Lengel [21] estimate a 5% error in the 1-1/1-0 ratio. Thus, in summary, the differences between the model and observed ratios fall within the combined error limits.…”

Section: Comparison With Model Spectra At 80 Kmmentioning

confidence: 99%

“…To resolve the relative contributions of these two sources present in the observed spectra, sets of synthetic spectra are required. The tabulations presented by Stevens and Conway [10] and Stevens et al [12] provide the rotational line wavelengths of the OH 0-0, 1-1, and 1-0 bands, the solar resonance rotational line g-factors of the 0-0 and 1-1 bands, and the relative rotational line intensities of the prompt emissions. The g-factors for the OH 1-0 band are determined assuming a 1-0 to 1-1 band ratio of 0.63, from Crosley and Lengel [21].…”

Section: Comparison With Model Spectra At 80 Kmmentioning

confidence: 99%

“…Individual rotational emission rate g-factors for solar resonance excitation of the 308 nm OH A 2 + -X 2 0-0 band were calculated by Stevens and Conway [10] in support of the Middle Atmosphere High-Resolution Spectrograph Investigation (MAHRSI) program. The precision of their derived values was clearly demonstrated by inter-comparison between observed and modelled rotational line intensities.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

OH A²Σ⁺ –X²Π band ratios observed in the mesosphere by OSIRIS

Gattinger¹,

Degenstein²,

Llewellyn³

et al. 2008

Can. J. Phys.

View full text Add to dashboard Cite

In this study, we present spectra of the mesospheric OH A 2 + -X 2 band system, including the 0-0, 1-1, and 1-0 bands, as observed by OSIRIS (Optical Spectrograph and Infrared Imaging System). Spectral components due to Rayleigh-scattered sunlight, lower thermospheric dayglow emission features, and baffle scatter have been removed to isolate the OH emission signature. The observed spectra are compared with model spectra assembled using rotational emission rate factors for solar resonance fluorescence (g-factors) plus prompt emission of the OH A 2 + -X 2 band system from solar Lyman-α photodissociation of water. The observed band ratios are in good agreement with the model values. The altitude variation of the 0-0 band, relative to the 1-1 band, is in agreement with model predictions based on vibrational energy transfer from OH A 2 + v = 1 to OH A 2 + v = 0. This detailed understanding of the OH A 2 + -X 2 system is critical for the successful application of OH observations to the determination of mesospheric OH densities and water vapor concentrations. PACS Nos.: 33.20.Lg, 33.20.Tp, 33.70.Fd, 92.60.hc, 92.60.hw Résumé : Nous présentons ici les résultats d'une étude du système de bande A 2 + -X 2 de l'OH mésosphérique, incluant les bandes 0-0, 1-1 et 1-0, tels que mesurés par OSIRIS (sytème de spectroscopie optique et d'imagerie infra-rouge embarqué sur Odin). Nous avons éliminé les composants spectraux dus à la diffusion Rayleigh de la lumière solaire, à la luminescence dans la basse thermosphère et à la diffusion de déflexion, afin de mieux isoler la signature des émissions OH. Les spectres observés sont comparés à des spectres composés en utilisant les taux d'émission pour la fluorescence résonante solaire (facteurs g) et l'émission spontanée du système de bande OH A 2 + v = 1 à OH A 2 + v = 0. La connaissance détaillée du système OH A 2 + -X 2 est critique dans l'utilisation des observations OH pour déterminer les densités OH et les concentrations de vapeur d'eau mésosphériques.[Traduit par la Rédaction]

show abstract

Section: Comparison With Model Spectra At 80 Kmmentioning

confidence: 99%

Section: Comparison With Model Spectra At 80 Kmmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

OH A²Σ⁺ –X²Π band ratios observed in the mesosphere by OSIRIS

Gattinger¹,

Degenstein²,

Llewellyn³

et al. 2008

Can. J. Phys.

View full text Add to dashboard Cite

show abstract

“…We express the fluorescence efficiency of each transition with the g factor, which is the number of solar photons scattered per second per OH molecule. The (0,0) rotational g factors were presented and compared to MAHRSI observations by Stevens and Conway [1999] and are not reproduced here. We first extend the work of Stevens and Conway by reporting the OH(1,1) rotational g factors near 314 nm.…”

Section: Emission Spectrum Of Oh A2σ+–x2πmentioning

confidence: 99%

“…Boldface entries indicate the brightest ten lines predicted in the (1,1) band. Summing over all rotational transitions, the vibrational band g factor at 200 K is calculated to be 5.3 × 10 −5 s −1 and in excellent agreement with the estimate by Stevens and Conway [1999] of 5.2 × 10 −5 s −1 . Using their 200 K g factor for the (0,0) band of 3.51 × 10 −4 s −1 , the calculated (1,1)/(0,0) band ratio for solar fluorescence is therefore 0.15 and in good agreement with airglow observations by OSIRIS [ Gattinger et al , 2008].…”

Section: Emission Spectrum Of Oh A2σ+–x2πmentioning

confidence: 99%

First UV satellite observations of mesospheric water vapor

et al. 2008

Self Cite

View full text Add to dashboard Cite

[1] We report the first UV satellite observations of mesospheric water vapor. The measurements are of nonthermal OH prompt emission between 300-330 nm produced directly from the photodissociation of water vapor by H Lyman-a. This technique is most sensitive to water vapor concentrations between 70-90 km altitude. We present OH data from two limb scanning experiments: the Middle Atmosphere High Resolution Spectrograph Investigation (MAHRSI) and the Optical Spectrograph and Infra-Red Imager System (OSIRIS). Interpretation of the lower resolution ($1 nm) OSIRIS spectra requires the rotational emission rate factors for OH(1,1) solar fluorescence between 313-318 nm, which we present for the first time herein. Comparison of water vapor concentration profiles with the most coincident profiles from the Halogen Occultation Experiment on the Upper Atmosphere Research Satellite shows agreement to within 30% between 75-80 km for both MAHRSI and OSIRIS. We discuss the benefits of this promising new approach to measuring upper mesospheric water vapor and the need for new laboratory measurements to improve the analysis.

show abstract

An unprecedented constraint on water content in the sunlit lunar exosphere seen by Lunar-based Ultraviolet Telescope of Chang׳e-3 mission

Wang

Qiu

et al. 2015

Planetary and Space Science

View full text Add to dashboard Cite

The content of OH/H 2 O molecules in the tenuous exosphere of the Moon is still an open issue at present. We here report an unprecedented upper limit of the content of the OH radicals, which is obtained from the in-situ measurements carried out by the Lunar-based Ultraviolet Telescope, a payload of Chinese Chang'e-3 mission. By analyzing the diffuse background in the images taken by the telescope, the column density and surface concentration of the OH radicals are inferred to be < 10 11 cm −2 and < 10 4 cm −3 (by assuming a hydrostatic equilibrium with a scale height of 100km), respectively, by assuming that the recorded background is fully contributed by their resonance fluorescence emission. The resulted concentration is lower than the previously reported value by about two orders of magnitude, and is close to the prediction of the sputtering model. In addition, the same measurements and method allow us to derive a surface concentration of < 10 2 cm −3 for the neutral magnesium, which is lower than the previously reported upper limit by about two orders of magnitude. These results are the best known of the OH (MgI) content in the lunar exosphere to date.

show abstract

Calculated OH A²Σ⁺−X²Π (0,0) band rotational emission rate factors for solar resonance fluorescence

Cited by 13 publications

References 31 publications

OH A²Σ⁺ –X²Π band ratios observed in the mesosphere by OSIRIS

OH A²Σ⁺ –X²Π band ratios observed in the mesosphere by OSIRIS

First UV satellite observations of mesospheric water vapor

An unprecedented constraint on water content in the sunlit lunar exosphere seen by Lunar-based Ultraviolet Telescope of Chang׳e-3 mission

Contact Info

Product

Resources

About

Calculated OH A2Σ+−X2Π (0,0) band rotational emission rate factors for solar resonance fluorescence

Cited by 13 publications

References 31 publications

OH A2Σ+ –X2Π band ratios observed in the mesosphere by OSIRIS

OH A2Σ+ –X2Π band ratios observed in the mesosphere by OSIRIS

First UV satellite observations of mesospheric water vapor

An unprecedented constraint on water content in the sunlit lunar exosphere seen by Lunar-based Ultraviolet Telescope of Chang׳e-3 mission

Contact Info

Product

Resources

About

Calculated OH A²Σ⁺−X²Π (0,0) band rotational emission rate factors for solar resonance fluorescence

OH A²Σ⁺ –X²Π band ratios observed in the mesosphere by OSIRIS

OH A²Σ⁺ –X²Π band ratios observed in the mesosphere by OSIRIS