Updated line parameters for OH X2II–X2II (ν′',ν′) Transitions

Goldman, A.; Schoenfeld, W.G.; Goorvitch, D.; Chackerian, C.; Dothe, H.; Mélen, F.; Abrams, M. C.; Selby, John E.

doi:10.1016/s0022-4073(97)00112-x

Cited by 116 publications

(115 citation statements)

References 32 publications

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“…However, it was recently noted by Cosby and Slanger 27 that the experimental data of Krassovsky et al 28 underlying part of that fit is seriously flawed by modern standards. A new set of emission rates was published by Goldman et al 29 in 1998, based on a Rydberg-Klein-Rees ͑RKR͒ potential of Nelson and Nesbitt. 30 The dipole moment function was obtained by combining an experimentally determined electric dipole moment function of Nelson et al 31 with an ab initio dipole moment of Goldman et al 29 An empirical spin-orbit coupling function by Coxon and Foster 32 was also included in that calculation.…”

Section: Introductionmentioning

confidence: 99%

Theoretical transition probabilities for the OH Meinel system

Loo

Groenenboom

2007

The Journal of Chemical Physics

138

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The authors present a new potential energy curve, electric dipole moment function, and spin-orbit coupling function for OH in the X 2 ⌸ state, based on high-level ab initio calculations. These properties, combined with a spectroscopically parametrized lambda-type doubling Hamiltonian, are used to compute the Einstein A coefficients and photoabsorption cross sections for the OH Meinel transitions. The authors investigate the effect of spin-orbit coupling on the lifetimes of rovibrationally excited states. Comparing their results with earlier ab initio calculations, they conclude that their dipole moment and potential energy curve give the best agreement with experimental data to date. The results are made available via EPAPS Document No. E-JCPSAG-017709.

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Section: Introductionmentioning

confidence: 99%

Theoretical transition probabilities for the OH Meinel system

Loo

Groenenboom

2007

The Journal of Chemical Physics

138

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“…The population distribution of the vibrational levels for the OH upper state X 2 P 3/2 has characteristics of a Boltzmann distribution with [Goldman et al, 1998]. Therefore, the ratio of the OH (4-0) to the total hydroxyl emissions is ∼0.0001, which is comparable to the result of ∼0.0002 derived from the observation data listed by Khomich et al [2008, Table 2.14].…”

Section: Sprite Emissions In the 762 Nm Passbandmentioning

confidence: 68%

The 762 nm emissions of sprites

et al. 2011

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[1] We report the 762 nm emissions in sprites recorded by the ISUAL experiment onboard the FORMOSAT-2 satellite. The 762 nm imager filter is centered at 763.3 nm with a 7 nm bandwidth at 50% transmittance. Sprite emissions in this passband include the N 2 first positive (1PN 2 ) bands, (2, 0) and (3, 1), the O 2 atmospheric (atm) band (0, 0), and the hydroxyl (4, 0) emissions. Because these mixed emissions cannot be resolved in the 762 nm narrowband filter, a zero-dimensional plasma chemistry model is used to estimate the expected relative intensities of these emission bands in sprites. The computed 1PN 2 brightness in a single streamer is 1.4 MR and 2.6 kR for the O 2 atm band emissions at frame integration times of 30 ms. In the 762 nm passband, the 1PN 2 emissions are the dominant emissions in sprites, and the ratio of 1PN 2 to O 2 atmospheric emissions is ∼500, while the hydroxyl emissions can be neglected. In this ISUAL 762 nm campaign, the brightest sprite out of the four recorded events has possible O 2 atm band emissions that lasted more than 90 ms, and its observed brightness is consistent with the model prediction. Even though the lightning 762 nm emissions are strongly absorbed by O 2 below 60 km, the ISUAL observed parent lightning emissions in this passband are still more than a factor of two brighter than those from ISUAL observed sprites. Hence for spacecraft nadir TLE detection missions, 762 nm bands may not be used as the sole signature to identify sprites, and auxiliary emission bands are needed.

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“…It is based on the laboratory work of Abrams et al (1994), complemented with the theoretical line list by Goldman et al (1998). The molecular gf-values of the OH lines were obtained from the Einstein coefficients calculated by Goldman et al (1998). The CN and CO infrared line lists were implemented in Meléndez & Barbuy (1999).…”

Section: Molecular Line Opacitiesmentioning

confidence: 99%

A library of high resolution synthetic stellar spectra from 300 nm to 1.8 ${\rm \mu}$m with solar andα-enhanced composition

Coelho¹,

Barbuy²,

Meléndez³

et al. 2005

A&A

392

498

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Libraries of stellar spectra are fundamental tools for the study of stellar populations, and both empirical and synthetic libraries have been used for this purpose. In this paper, a new library of high resolution synthetic spectra is presented, ranging from the near-ultraviolet (300 nm) to the near-infrared (1.8 µm). The library spans all the stellar types that are relevant to the integrated light of old and intermediate-age stellar populations in the involved spectral region (spectral types F through M and all luminosity classes). The grid was computed for metallicities ranging from [Fe/H] = -2.5 to +0.5, including both solar and α-enhanced ([α/Fe] = 0.4) chemical compositions. The synthetic spectra are a good match to observations of stars throughout the stellar parameter space encompassed by the library and over the whole spectral region covered by the computations.

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Updated line parameters for OH X2II–X2II (ν′',ν′) Transitions

Cited by 116 publications

References 32 publications

Theoretical transition probabilities for the OH Meinel system

Theoretical transition probabilities for the OH Meinel system

The 762 nm emissions of sprites

A library of high resolution synthetic stellar spectra from 300 nm to 1.8 ${\rm \mu}$m with solar andα-enhanced composition

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