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

Gattinger, R. L.; Degenstein, D. A.; Llewellyn, E. J.; Stevens, M. H.

doi:10.1139/p08-015

Cited by 4 publications

(8 citation statements)

References 20 publications

(27 reference statements)

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“…At 318.5 nm (OS pixels 112-114), the OS can detect Rayleigh-scattered sunlight, with insignificant baffle scatter contamination, up to tangent heights of ∼ 85-90 km. This wavelength region also avoids contamination from emission in the nearby OH (A 2 → X 2 ) (1 − 1) band near 314 nm (Gattinger et al, 2008) and from the N 2 (C 3 u → B 3 g ) (1 − 0) band near 316 nm (Cleary et al, 1995). However, at 318.5 nm O 3 absorption along the OSIRIS line-of-sight can become significant below ∼ 65 km.…”

Section: Osiris Temperaturesmentioning

confidence: 98%

Assessment of the quality of OSIRIS mesospheric temperatures using satellite and ground-based measurements

et al. 2012

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The Optical Spectrograph and InfraRed Imaging System (OSIRIS) on the Odin satellite is currently in its 12th year of observing the Earth's limb. For the first time, continuous temperature profiles extending from the stratopause to the upper mesosphere have been derived from OSIRIS measurements of Rayleigh-scattered sunlight. Through most of the mesosphere, OSIRIS temperatures are in good agreement with coincident temperature profiles derived from other satellite and ground-based measurements. In the altitude region of 55-80 km, OSIRIS temperatures are typically within 4-5 K of those from the SABER, ACE-FTS, and SOFIE instruments on the TIMED, SciSat-I, and AIM satellites, respectively. The mean differences between individual OSIRIS profiles and those of the other satellite instruments are typically within the combined uncertainties and previously reported biases. OSIRIS temperatures are typically within 2 K of those from the University of Western Ontario's Purple Crow Lidar in the altitude region of 52-79 km, where the mean differences are within combined uncertainties. Near 84 km, OSIRIS temperatures exhibit a cold bias of 10-15 K, which is due to a cold bias in OSIRIS O 2 A-band temperatures at 85 km, the upper boundary of the Rayleigh-scatter derived temperatures; and near 48 km OSIRIS temperatures exhibit a cold bias of 5-15 K, which is likely due to multiple-scatter effects that are not taken into account in the retrieval.

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Section: Osiris Temperaturesmentioning

confidence: 98%

Assessment of the quality of OSIRIS mesospheric temperatures using satellite and ground-based measurements

et al. 2012

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“…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%

“…The relative intensity of the (0,0) band in black is shown against the (1,1) band in red at 200 K, where the rotational emission rate factors ( g factors) are indicated on the y axis. Below ∼70 km, the (0,0)/(1,1) ratio changes due to vibrational energy transfer within the upper electronic state [ Gattinger et al , 2008]. The entire spectrum is smoothed using the OSIRIS spectral resolution function with a full‐width at half‐maximum of ∼1 nm (scaled arbitrarily).…”

Section: Emission Spectrum Of Oh A2σ+–x2πmentioning

confidence: 99%

“…The volume emission rate ( P ) can be expressed as where ψ λ ( z ) is the H Lyman‐ α flux at each altitude level, ϕ is the OH(0,0) + (1,1) prompt yield, σ λ is the water vapor cross section and [ H 2 O ( z )] is the water vapor concentration [ Gumbel , 1997]. In our modeling approach, we neglect quenching of the A 2 Σ + state as well as vibrational energy transfer (VET) and rotational energy transfer (RET), which become important below ∼65 km [ Conway et al , 1999; Gattinger et al , 2008]. Available laboratory results indicate, moreover, that quenching and RET are less efficient at high rotational levels (N′ = 16–20) than at low rotational levels (N′ < 3) [ Kaneko et al , 1968; Copeland et al , 1985; Papagiannakopoulos and Fotakis , 1985; Burris et al , 1991; Gumbel , 1997].…”

Section: Modeling Approachmentioning

confidence: 99%

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First UV satellite observations of mesospheric water vapor

et al. 2008

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[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.

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“…It is also modulated by background atmospheric temperature and [H].Recently, observations of the OH dayglow intensity at Thumba (8.5°N, 77°E) using a dayglow photometer have been reported [Pant et al, 2004[Pant et al, , 2007Kumar et al, 2008] and used to study waves at the equator. In addition, the OH dayglow has been observed from space by the TIMED (Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics) and Odin satellites [Gattinger et al, 2008]. By means of the TIMED/ SABER (Sounding of the Atmosphere using Broadband Emission Radiometry) OH dayglow observation, GAO ET AL.DOUBLE-LAYER STRUCTURE OF OH DAYGLOW 5778 PUBLICATIONS (2015), Double-layer structure of OH dayglow in the mesosphere,…”

mentioning

confidence: 99%

Double‐layer structure of OH dayglow in the mesosphere

Gao

Ward

et al. 2015

JGR Space Physics

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Observations by the Sounding of the Atmosphere using Broadband Emission Radiometry instrument on the Thermosphere‐Ionosphere‐Mesosphere Energetics and Dynamics satellite from January 2002 to June 2014 are used to study the vertical structure of OH dayglow. The results indicate for the first time that there is a double‐layer structure in the distributions of 12 year averaged OH airglow emission, [O3], and [H] during the daytime. The upper layer of OH dayglow is located in the mesopause region (~88 km) at a similar altitude to that of the OH nightglow. The lower layer is situated in the range of 70–85 km. Both the peak emission and height of the lower layer increase with local time. The distance between the two layers decreases with local time. At the equator, the lower layer forms at ~09:00 LT and lasts for about 8 h; during this time the interlayer distance decreases from 13 km to 5 km. The double‐layer structure is more obvious and longer‐lived during the equinoxes and at lower latitudes. The double‐layer structure of OH dayglow emission is a long‐term stable structure and is mainly caused by photochemical processes involving [O3]. It is also modulated by background atmospheric temperature and [H].

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

Cited by 4 publications

References 20 publications

Assessment of the quality of OSIRIS mesospheric temperatures using satellite and ground-based measurements

Assessment of the quality of OSIRIS mesospheric temperatures using satellite and ground-based measurements

First UV satellite observations of mesospheric water vapor

Double‐layer structure of OH dayglow in the mesosphere

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