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Relevant bibliographies by topics / OH meinel band

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Academic literature on the topic 'OH meinel band'

Author: Grafiati

Published: 6 September 2023

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Journal articles on the topic "OH meinel band"

1

Fagundes, P. R., D. Gobbi, H. Takahashi, and Y. Sahai. "Mesospheric energy loss rates by OH and O<sub>2</sub> emissions at 23<sup>°</sup>S." Annales Geophysicae 15, no. 6 (June 30, 1997): 797–804. http://dx.doi.org/10.1007/s00585-997-0797-4.

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Abstract. The nightglow OH(9, 4) and O2 atmospheric (0,1) band emission intensities and their rotational temperatures T(OH) and T(O2), respectively, observed at Cachoeira Paulista (23°S, 45°W), Brazil, during the period from October 1989 to December 1990, have been analyzed to study the nighttime mesospheric energy loss rates through the radiations from the vibrationally excited OH* and electronically excited O2* bands. The total emission rates of the OH Meinel bands, O2 atmospheric (0,0) and O2 infrared atmospheric (1Δg) bands were calculated using reported data for the relative band intensities I(ν'',ν')/I(9,4), IO2A(0,0)/IO2A(0,1) and IO2(1Δg)/IO2A(0,1). It was found that there is a minimum in equivalent energy loss rate by the OH* Meinel bands during December/January (equivalent energy loss rate of 0.39K/day*, where day* means averaged over the night) and maximum in equivalent energy loss rate during September (equivalent energy loss rate of 0.98K/day*). Energy loss rate by the O2* radiation, on the other hand, is weaker than that by the OH* Meinel bands, showing equivalent energy loss rates of 0.12K/day* and 0.22K/day* during January and September, respectively.

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Parihar, N., A. Taori, S. Gurubaran, and G. K. Mukherjee. "Simultaneous measurement of OI 557.7 nm, O<sub>2</sub> (0, 1) Atmospheric Band and OH (6, 2) Meinel Band nightglow at Kolhapur (17° N), India." Annales Geophysicae 31, no. 2 (February 7, 2013): 197–208. http://dx.doi.org/10.5194/angeo-31-197-2013.

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Abstract. Near-simultaneous measurements of OI 557.7 nm, O2 (0, 1) Atmospheric Band and OH (6, 2) Meinel Band nightglow were carried out at Kolhapur (17° N), India during February–March 2007. Atmospheric temperatures around 87 and 94 km were derived from the knowledge of intensity measurements of spectral features OH (6, 2) Meinel Band and O2 Atmospheric Band, respectively. An account of the behaviour of derived temperatures has been presented. The nocturnal behaviour of OH and O2 temperatures is governed by the waves of tidal origin, whereas the signatures of planetary wave-like oscillations is noted in the night-to-night variation of two temperatures. This is probably the first report of planetary waves observed in nightglow temperatures from the Indian subcontinent.

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Sheese, P. E., E. J. Llewellyn, R. L. Gattinger, and K. Strong. "OH Meinel band nightglow profiles from OSIRIS observations." Journal of Geophysical Research: Atmospheres 119, no. 19 (October 3, 2014): 11,417–11,428. http://dx.doi.org/10.1002/2014jd021617.

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von Savigny, C., I. C. McDade, K. U. Eichmann, and J. P. Burrows. "On the dependence of the OH<sup>*</sup> Meinel emission altitude on vibrational level: SCIAMACHY observations and model simulations." Atmospheric Chemistry and Physics Discussions 12, no. 2 (February 23, 2012): 5817–49. http://dx.doi.org/10.5194/acpd-12-5817-2012.

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Abstract. Measurements of the OH Meinel emissions in the terrestrial nightglow are one of the standard ground-based techniques to retrieve upper mesospheric temperatures. It is often assumed that the emission peak altitudes are not strongly dependent on the vibrational level, although this assumption is not based on convincing experimental evidence. In this study we use Envisat/SCIAMACHY (Scanning Imaging Absorption spectroMeter for Atmospheric CHartographY) observations in the near-IR spectral range to retrieve vertical volume emission rate profiles of the OH(3-1), OH(6-2) and OH(8-3) Meinel bands in order to investigate, whether systematic differences in emission peak altitudes can be observed between the different OH Meinel bands. The results indicate that the emission peak altitudes are different for the different vibrational levels, with bands originating from higher vibrational levels having higher emission peak altitudes. It is shown that this finding is consistent with the majority of the previously published results. The SCIAMACHY observations yield differences in emission peak altitudes of up to about 4 km between the OH(3-1) and the OH(8-3) band. The observations are complemented by model simulations of the fractional population of the different vibrational levels and of the vibrational level dependence of the emission peak altitude. The model simulations well reproduce the observed vibrational level dependence of the emission peak altitude – both qualitatively and quantitatively – if quenching by atomic oxygen as well as multi-quantum collisional relaxation by O2 is considered. If a linear relationship between emission peak altitude and vibrational level is assumed, then a peak altitude difference of roughly 0.5 km per vibrational level is inferred from both the SCIAMACHY observations and the model simulations.

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von Savigny, C., I. C. McDade, K. U. Eichmann, and J. P. Burrows. "On the dependence of the OH<sup>*</sup> Meinel emission altitude on vibrational level: SCIAMACHY observations and model simulations." Atmospheric Chemistry and Physics 12, no. 18 (September 28, 2012): 8813–28. http://dx.doi.org/10.5194/acp-12-8813-2012.

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Abstract. Measurements of the OH Meinel emissions in the terrestrial nightglow are one of the standard ground-based techniques to retrieve upper mesospheric temperatures. It is often assumed that the emission peak altitudes are not strongly dependent on the vibrational level, although this assumption is not based on convincing experimental evidence. In this study we use Envisat/SCIAMACHY (Scanning Imaging Absorption spectroMeter for Atmospheric CHartographY) observations in the near-IR spectral range to retrieve vertical volume emission rate profiles of the OH(3-1), OH(6-2) and OH(8-3) Meinel bands in order to investigate whether systematic differences in emission peak altitudes can be observed between the different OH Meinel bands. The results indicate that the emission peak altitudes are different for the different vibrational levels, with bands originating from higher vibrational levels having higher emission peak altitudes. It is shown that this finding is consistent with the majority of the previously published results. The SCIAMACHY observations yield differences in emission peak altitudes of up to about 4 km between the OH(3-1) and the OH(8-3) band. The observations are complemented by model simulations of the fractional population of the different vibrational levels and of the vibrational level dependence of the emission peak altitude. The model simulations reproduce the observed vibrational level dependence of the emission peak altitude well – both qualitatively and quantitatively – if quenching by atomic oxygen as well as multi-quantum collisional relaxation by O2 is considered. If a linear relationship between emission peak altitude and vibrational level is assumed, then a peak altitude difference of roughly 0.5 km per vibrational level is inferred from both the SCIAMACHY observations and the model simulations.

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Parihar, Navin, Dupinder Singh, and Subramanian Gurubaran. "A comparison of ground-based hydroxyl airglow temperatures with SABER/TIMED measurements over 23° N, India." Annales Geophysicae 35, no. 3 (March 7, 2017): 353–63. http://dx.doi.org/10.5194/angeo-35-353-2017.

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Abstract. Ground-based observations of OH (6, 2) Meinel band nightglow were carried out at Ranchi (23.3° N, 85.3° E), India, during January–March 2011, December 2011–May 2012 and December 2012–March 2013 using an all-sky imaging system. Near the mesopause, OH temperatures were derived from the OH (6, 2) Meinel band intensity information. A limited comparison of OH temperatures (TOH) with SABER/TIMED measurements in 30 cases was performed by defining almost coincident criterion of ±1.5° latitude–longitude and ±3 min of the ground-based observations. Using SABER OH 1.6 and 2.0 µm volume emission rate profiles as the weighing function, two sets of OH-equivalent temperature (T1. 6 and T2. 0 respectively) were estimated from its kinetic temperature profile for comparison with OH nightglow measurements. Overall, fair agreement existed between ground-based and SABER measurements in the majority of events within the limits of experimental errors. Overall, the mean value of OH-derived temperatures and SABER OH-equivalent temperatures were 197.3 ± 4.6, 192.0 ± 10.8 and 192.7 ± 10.3 K, and the ground-based temperatures were 4–5 K warmer than SABER values. A difference of 8 K or more is noted between two measurements when the peak of the OH emission layer lies in the vicinity of large temperature inversions. A comparison of OH temperatures derived using different sets of Einstein transition probabilities and SABER measurements was also performed; however, OH temperatures derived using Langhoff et al. (1986) transition probabilities were found to compare well.

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Kalogerakis, Konstantinos S. "A previously unrecognized source of the O2Atmospheric band emission in Earth’s nightglow." Science Advances 5, no. 3 (March 2019): eaau9255. http://dx.doi.org/10.1126/sciadv.aau9255.

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Earth’s night sky continuously produces a faint chemiluminescence known as nightglow. Two prominent nighttime emissions around 90 km are the O2Atmospheric and the OH Meinel band systems. Despite a plethora of studies since their identification seven decades ago, substantial gaps persist in our understanding of the mechanisms that control them. This report shows that oxygen atoms connect these two emissions: Fast, multiquantum, vibrational-to-electronic relaxation of OH(v) by O atoms activates a pathway that generates O2Atmospheric band emission. This newly discovered source exhibits a strong altitude dependence and can contribute a majority of the observed O2Atmospheric band emission when the peaks of the OH and O-atom layers overlap. The new findings call for a reinterpretation of Earth’s nightglow emissions and a revision of relevant atmospheric models.

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Murtagh, D. P., J. Stegman, G. Witt, E. J. Llewellyn, and I. C. McDade. "A twilight measurement of the OH(8-3) meinel band and atmospheric temperature." Planetary and Space Science 35, no. 9 (September 1987): 1149–55. http://dx.doi.org/10.1016/0032-0633(87)90021-3.

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McDade, I. C., and E. J. Llewellyn. "Mesospheric oxygen atom densities inferred from night-time OH Meinel band emission rates." Planetary and Space Science 36, no. 9 (September 1988): 897–905. http://dx.doi.org/10.1016/0032-0633(88)90097-9.

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Parihar, N., S. Gurubaran, and G. K. Mukherjee. "Observations of OI 557.7 nm nightglow at Kolhapur (17° N), India." Annales Geophysicae 29, no. 10 (October 25, 2011): 1873–84. http://dx.doi.org/10.5194/angeo-29-1873-2011.

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Abstract. Ground-based nightglow observations of the atomic oxygen green line at 557.7 nm have been carried out at a low latitude station Kolhapur (17° N), India, during November 2003–April 2004 and December 2004–May 2005. The nocturnal behaviour of OI 557.7 nm intensity and a comparative study with simultaneous OH Meinel band temperature measurements has been presented. OI 557.7 nm intensity and OH temperature variations covary on many occasions. It was found that an 8 h tide characterizes the variation of intensity and temperature on most nights, and especially during the month of January. This is the first report of prolonged measurements of OI 557.7 nm emission from India.

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Dissertations / Theses on the topic "OH meinel band"

1

Choi, Gi-Hyuk. "A study of the variability of dynamics and temperatures near the mesopause from observations of the hydroxyl (OH) Meinel band emissions." Thesis, University College London (University of London), 1996. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.244222.

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García, Muñoz Antonio. "Airglow on Mars : model predictions for the O2 IR atmospheric band at 1.27 [micrometers], the OH meinel bands and the OH A-X band system ; Physical and chemical aeronomy of HD 209458b /." 2006. http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&res_dat=xri:pqdiss&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&rft_dat=xri:pqdiss:NR19846.

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Thesis (Ph.D.)--York University, 2006. Graduate Programme in Earth and Space Science.
Typescript. Includes bibliographical references (leaves 207-226). Also available on the Internet. MODE OF ACCESS via web browser by entering the following URL: http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&res_dat=xri:pqdiss&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&rft_dat=xri:pqdiss:NR19846

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Yen-JungWu and 吳彥蓉. "The leading role of atomic oxygen in the height of the elves, the D-region ledge in nighttime electron density and the OH* Meinel band nightglow layer." Thesis, 2017. http://ndltd.ncl.edu.tw/handle/g6a6gz.

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博士
國立成功大學
物理學系
105
The Imager of Sprite and Upper Atmospheric Lightning, the scientific nighttime payload onboard the Taiwanese FORMOSAT 2 satellite, provides observations of TLEs and OH* Meinel nightglow simultaneously in limb view from 2004 to 2016, within the +/-60 degree latitude range of the satellite orbit. The physical connection between two optical phenomena occurring at a similar altitude in limb viewing opens another window to study the structure of this critical altitude range that has long been lacking in in situ measurements. The ISUAL positioning has now been calibrated by the precise location of stars, and the pointing accuracy of ISUAL from 2005 to the end of 2011 is estimated to be 0.05° when viewing the limb region from the satellite. ISUAL is the only space-borne instrument equipped for simultaneous observation of elves and OH* nightglow. For the limb elves, 91% of the 291 events are located within +/- 4 km of the altitude of brightest OH* nightglow emission. The Semiannual Oscillation (SAO) at low latitude is a significant feature of the OH* nightglow because of the resulting vertical transport of atomic oxygen affected by tidal motions and migration in the mesosphere. The elve heights show the same variation: higher in the solstice seasons and lower in the equinox seasons. Based on the observational truth of this collocation, the processes and mechanisms which have been questioned, or which have not been previously declared, are shown and discussed in this thesis: (1) The relation between elves and atomic oxygen: The environment-based electron density profile is adapted as the input to the conventional elve model [Kuo et al. [2007] to ascertain the brightest height of elve emission. Along with the OH*model from SABER analysis [Xu et al., 2012; Smith et al., 2012], the model results show clearly that both the height of elves and OH* nightglow are higher when the ledge of the atomic oxygen profile is higher, and vice versa. (2) The relation between the OH* nightglow and the electron density ledge: The semiannual oscillation driven by the vertical transport of atomic oxygen is primary evidence linking the altitudes of elves, OH* nightglow and the VLF waveguide boundary near 87 km [Toledo-Redondo et al., 2012]. The third question addressed in this work concerns the role of meteoric smoke particles in the electron density ledge when atomic oxygen serves to free the electrons from negative ions: Two measureables of the ED ledge are the height and the scale height, and are examined with 102 rocket soundings. One third of the soundings show a maximum frequency at 87 km and a mean scale height of 1.2 km. The size range for micrometeoroids estimated by the classical model for ablation onset overlaps remarkably well with the fixed height portions of the curves for meteor speeds of 10-20 km/s in the height range 80 to 90 km where the ED ledge, elve and OH* nightglow are all located. The concentration of MSPs, capable of reducing the electron density by scavenging, is estimated based on mass conservation. This estimate is of the same order as the measured electron density at 86 km, so that electron scavenging is plausible. Furthermore, the meteor velocity observations from the Jicamarca HPLA meteor radar have been used to show a gradual increase in counts (after correction of the velocity distribution according to the ionization probability β(V)) down to the terrestrial escape velocity of 11 km/s, where the laboratory measurements of β(V) lack access. In short, at the altitude where atomic oxygen is present, MSPs are required to make the electron density ledge. The leading role for atomic oxygen in determining the altitude of elves, OH* nightglow and the electron density profile along with MSPs has been verified by both observation and theoretical model. The observational truth of the collocation offers a new perspective on the composition, the photochemistry and the dynamics of the mesosphere where the transition region between the ionosphere and the neutral atmosphere is difficult to monitor and where new discoveries lie around the corner. Key words: Elves, OH* nightglow, D-region ionosphere, electron density, atomic oxygen

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Conference papers on the topic "OH meinel band"

1

Skinner, Wilbert R., and Jeng-Hwa Yee. "Wideband Filter Spectrophotometer for Mesospheric and Thermospheric Studies." In Optical Remote Sensing of the Atmosphere. Washington, D.C.: Optica Publishing Group, 1990. http://dx.doi.org/10.1364/orsa.1990.md8.

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The effect of small scale features, such as gravity waves, on the mesosphere and lower thermosphere is a subject of much current interest. One way to study these phenomenon is to monitor their effects on the airglow emissions originating in the region. Band emissions, such as the OH Meinel and O2 Atmospheric bands are particularly useful. Instrumentally these are difficult to study because of their wide spectral nature and low intensity. Often, it is necessary to infer the properties of an entire band from the observations of a few lines with either a filter photometer or a Fabry-Perot interferometer (Meriwether, 1975). Another approach has been to scan a band with a grating spectrometer, a process that is often slow compared to many of the temporal features of interest (Myrabo and Deehr, 1984).

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Nelson, D. D., M. S. Zahniser, and J. Wormhoudt. "Quantitative IR spectroscopy of atmospheric and combustion radicals with comparison to theory." In OSA Annual Meeting. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/oam.1992.wl3.

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Infrared laser absorption techniques have been employed to measure absolute transition moments for several radical species by using a variety of techniques. For the OH radical, high precision relative transition strengths have been measured with a color center laser and used to determine the OH dipole moment function. The dipole moment function provides absolute transition strengths for Δv = 1–3 transitions with v″ < 9. This information is essential for quantitative modelling of the OH Meinel night glow. The infrared band strengths for all three fundamental vibrations of the HO2 radical have been directly measured by using tunable infrared diode laser absorption. The HO2 radicals were prepared with a known column density by reacting a known quantity of F atoms with excess H2O2. These band strengths will be used to measure HO2 radical concentrations in the troposphere. Band strengths for the BF, CF2, and CH3 radicals have also been obtained using tunable diode laser absorption. These species' concentrations were quantified by by using various optical and chemical techniques. The experimental infrared transition strengths discussed above will be compared with published theoretical transition strengths obtained by using several techniques.

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Abrams, Mark C., Sumner P. Davis, and Rolf Engleman. "High-resolution spectroscopy of the Meinel bands of OH and OD." In OSA Annual Meeting. Washington, D.C.: Optica Publishing Group, 1988. http://dx.doi.org/10.1364/oam.1988.mr21.

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The IR spectrum of the Meinel bands of the OH and OD free radicals was observed in a cold ozone-hydrogen diffusion flame using the Fourier transform spectrometer at the National Solar Observatory (Kitt Peak). Eighteen bands have been observed in the spectral region between 1900 and 9000 cm-1. Wavenumbers, intensities, line shapes, and isotope shifts have been obtained. The spectrum has been synthesized and optimal molecular parameters obtained using molecular Hamiltonians and nonlinear least-squares fitting techniques. The same spectrum has been observed in two other sources, the inductively coupled plasma and the oxyacetylene flame. Comparisons of the three spectra are being made.

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Davis, Sumner P., Rolf Engleman, and Mark C. Abrams. "Fourier Transform Spectroscopy of OH and OD in the Infrared." In High Resolution Fourier Transform Spectroscopy. Washington, D.C.: Optica Publishing Group, 1989. http://dx.doi.org/10.1364/hrfts.1989.wa2.

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We are making a thorough study of the Meinel bands of OH and OD radicals in the spectral region 1900 to 9000 cm−1. Three sources have been used, the ozone-hydrogen flame, the oxygen-acetylene flame, and the inductively coupled plasma (ICP). Differences in the spectra are immediately apparent, as shown in Figure 1. The ozone-hydrogen flame operates at low pressure, the lines are sharp, and the excitation is non-thermal. The oxygen-acetylene flame operates at atmospheric pressure and produces thermal excitation and broad lines. The ICP spectrum is similar to the oxygen-acetylene flame but with lines of intermediate sharpness.

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Abrams, Mark C., Sumner P. Davis, and Rolf Engleman. "High resolution spectroscopy of the OH and OD free radicals produced in an inductively coupled plasma discharge." In OSA Annual Meeting. Washington, D.C.: Optica Publishing Group, 1989. http://dx.doi.org/10.1364/oam.1989.tugg5.

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The infrared spectrum of the Meinel bands of the OH and OD free radicals was observed in an inductively coupled plasma (ICP) using the McMath Fourier transform spectrometer at the National Solar Observatory (Kitt Peak). Wavenumbers, intensities, line shapes, and isotope shifts have been determined. The spectrum has been synthesized and optimum molecular parameters obtained using molecular Hamiltonians and nonlinear least-squares fitting techniques. Rotational temperature determinations provide plasma diagnostics in the outer sheath of the plasma.

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