Abundances of carbon-bearing diatomic molecules in diffuse interstellar clouds

Dickman, R. L.; Somerville, W. B.; Whittet, D. C. B.; McNally, D.; Blades, J. C.

doi:10.1086/190883

Cited by 25 publications

(9 citation statements)

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“…Strong molecular lines were found for only a few lines of sight, although marginal detections were reported toward about half of the stars. In subsequent years, additional translucent clouds have been found through searches either for the absorption lines of the CH, CH+ or CN molecules at blue wavelengths (Blades and Bennewith 1973; Dickman et al 1983;Crutcher and Chu 1985;Cardelli and Wallerstein 1986), or for lines of the C2 molecule at red wavelengths (Souza and Lutz 1977; Hobbs, Black, and van Dishoeck 1983; Lutz and Crutcher 1983; van Dishoeck and de Zeeuw 1984; Gredel and Munch 1986;Jannuzi et al 1988;Federman and Lambert 1988). Millimeter emission line studies are lacking for most of these clouds.…”

Section: Introductionmentioning

confidence: 99%

Interstellar C2, CH, and CN in translucent molecular clouds

Dishoeck¹,

Black²

1989

ApJ

137

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Optical absorption line techniques have been applied to the study of a number of translucent molecular clouds in which the total column densities are large enough that substantial molecular abundances can be maintained. Results are presented for a survey of absorption lines of interstellar C2, CH, and CN. Detections of CN through the A2II-X2E+ (1,0) and (2,0) bands of the red system are reported, and are compared with observations of the blue system for one line of sight. The population distributions in C2 provide diagnostic information on temperature and density. The measured column densities of the three species can be used to test details of the theory of molecule formation in clouds where photo-processes still play a significant role. The C2 and CH column densities are strongly correlated with each other and probably also with the H2 column density. In contrast, the CN column densities are found to vary greatly from cloud to cloud. The observations are discussed with reference to detailed theoretical models.

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Section: Introductionmentioning

confidence: 99%

Interstellar C2, CH, and CN in translucent molecular clouds

Dishoeck¹,

Black²

1989

ApJ

137

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“…The former effect could be due to K -type resonance, as in NCO (23). However, Brazier et al note that they were unable to fit any transitions involving levels with J < 9.5 in the F 2 component of the (110) 2 level in their analysis. We are also unable to make any assignments at low J in the F 2 subband.…”

Section: Discussionmentioning

confidence: 97%

“…It is astrophysically important because a large number of carbon-containing chain species have been observed in the interstellar medium (1). Both CN (2) and CCCN (3) have been detected in interstellar clouds and in stellar envelopes (although CCN itself has not been observed to date). CCN is also thought to be involved in combustion processes in fuel-rich natural gas flames (4).…”

Section: Introductionmentioning

confidence: 99%

The Infrared Laser Spectrum of the 101211 Hot Band of CCN

Beaton¹,

Gillett²,

Brown³

et al. 2001

Journal of Molecular Spectroscopy

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“…The reaction of N( 4 S ) + CH( X 2 П) → H( 2 S ) + CN ( X 2 Σ + , A 2 П) plays an important role in interstellar chemistry as one of primary sources of CN radicals which is an important intermediate product in the N 2 formation . It is also involved in atmosphere and combustion chemistry .…”

Section: Reaction Dynamics Of N(4s) + Ch(x2п) → H(2s) + Cn (X2σ+ A2п)mentioning

confidence: 99%

State‐to‐state reaction dynamics for the reactions of atom N with radicals

Xie

2014

Int J of Quantum Chemistry

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Much progress has been achieved in the developments of accurate and efficient algorithms for quantum dynamics calculations in the past two decades. Based on the reliable potential energy surfaces (PESs) constructed with state-of-the-art ab initio calculations, quantum reactive scattering calculations for the atom-diatom collisions can be performed accurately at the state-to-state level. In this review, we described the general strategies of constructing a PES and the Chebyshev real wave packet method briefly, and summarized our recent studies on the PESs and state-to-state reaction dynamics for the reactions of the atom N with radicals OH, CH, and C 2 . Such barrierless complex-forming reactions are very important for understanding low-temperature reaction dynamics and still difficult to treat accurately.

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Abundances of carbon-bearing diatomic molecules in diffuse interstellar clouds

Cited by 25 publications

References 0 publications

Interstellar C2, CH, and CN in translucent molecular clouds

Interstellar C2, CH, and CN in translucent molecular clouds

The Infrared Laser Spectrum of the 101211 Hot Band of CCN

State‐to‐state reaction dynamics for the reactions of atom N with radicals

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