Infrared Spectra of Acetylene Diluted in Solid Nitrogen Upon Irradiation With Vacuum Ultraviolet Light and Electrons

Wu, Yu-Jong; Chuang, Shiang-Jiun; Chen, Sian-Cong; Huang, Tzu-Ping

doi:10.1088/0067-0049/212/1/7

Cited by 13 publications

(5 citation statements)

References 44 publications

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“…The experimental setup has been described previously. ,, IR absorption spectra covering the spectral range 450–5000 cm –1 were recorded with an interferometric spectrometer (Bruker v80) equipped with a KBr beamsplitter and a Hg–Cd–Te detector cooled to 77 K. Typically 400 scans at a resolution of 0.5 cm –1 were recorded in each stage of an experiment.…”

Section: Methodsmentioning

confidence: 99%

Photoisomerization and Infrared Spectra of Allene and Propyne Cations in Solid Argon

Liu

Chen

Chin

et al. 2015

J. Phys. Chem. Lett.

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Allene and propyne as well as their cationic forms play important roles in combustion and interstellar chemistry and serve as a model system for molecular spectroscopic studies. Both cations show Jahn−Teller (J−T) distortions in their ground states. These J−T distortions make the theoretical and experimental studies of their electronic structures difficult. We produced allene cations upon electron bombardment during matrix deposition of Ar containing a small proportion of allene. The intensities of the absorption features of the allene cation decreased after irradiation with UV light, whereas new bands attributed to propyne cations increased. The observed line wavenumbers, relative intensities, and deuterium-substituted isotopic ratios of the isomers of C 3 H 4 + agree satisfactorily with those predicted by density functional theory at the B3PW91/ aug-cc-pVTZ level of theory. This method produced the hydrocarbon cations of interest with few other fragments that enabled the clear identification of the IR spectra of allene and propyne cations.

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Section: Methodsmentioning

confidence: 99%

Photoisomerization and Infrared Spectra of Allene and Propyne Cations in Solid Argon

Liu

Chen

Chin

et al. 2015

J. Phys. Chem. Lett.

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“…Outside of astrochemistry the photo production of radicals in CO, N 2 , and noble gas matrices has been studied for many decades, − to spectroscopically identify and characterize unstable species; matrix isolation enables the long-time survival of highly reactive radicals and results in very narrow infrared line widths, which together makes matrix isolation an excellent tool for radical characterization. In this subsection we review the outcome of photochemistry experiments on CH 3 OH in CO ices, CH 4 in N 2 and CO ices, H 2 S in CO (and CO 2 ) ice, ethylene, methane and acetylene in N 2 ice, − and H 2 CO in noble gas matrices . Some of these experiments involve UV energy resolved data, which provides additional constraints on the formation mechanisms.…”

Section: Photochemistry In Simple/binary Ice Mixturesmentioning

confidence: 99%

“…One clue may by that HCN and HNC do not form in C 2 H 2 :N 2 photolysis experiments. This result has been taken as evidence that a critical minimum H atom production rate is needed in the ice for efficient HCN and HNC formation. − An alternative explanation is that these molecules only form through reactions with N 2 and CH 2 and CH 3 , and not through reactions between N 2 and CH or C. This hypothesis could be tested by adding H 2 to the C 2 H 2 ice experiment and determining the initial product yield (before any more saturated hydrocarbons or radicals have formed).…”

Section: Photochemistry In Simple/binary Ice Mixturesmentioning

confidence: 99%

Photochemistry and Astrochemistry: Photochemical Pathways to Interstellar Complex Organic Molecules

2016

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The interstellar medium is characterized by a rich and diverse chemistry. Many of its complex organic molecules are proposed to form through radical chemistry in icy grain mantles.Radicals form readily when interstellar ices (composed of water and other volatiles) are exposed to UV photons and other sources of dissociative radiation, and if sufficiently mobile the radicals can react to form larger, more complex molecules. The resulting complex organic molecules (COMs) accompany star and planet formation, and may eventually seed the origins of life on nascent planets. Experiments of increasing sophistication have demonstrated that known interstellar COMs as well as the prebiotically interesting amino acids can form through ice photochemistry. We review these experiments and discuss the qualitative and quantitative kinetic and mechanistic constraints they have provided. We finally compare the effects of UV radiation with those of three other potential sources of radical production and chemistry in interstellar ices: electrons, ions and X-rays.

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“…The release of these compounds to gas phase by thermal evaporation, photo-desorption, or sputtering would produce an increase in the abundance of nitriles (CN, HCN, and HNC). Subsequent experiments show that nitriles can also be produced by irradiation of ices formed with N 2 and other C-bearing species such as acetylene (Wu et al 2014;Chen et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Linking the dust and chemical evolution: Taurus and Perseus

Bop

Lique

Esplugues

et al. 2023

A&A

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Context. HCN, HNC, and their isotopologues are ubiquitous molecules that can serve as chemical thermometers and evolutionary tracers to characterize star-forming regions. Despite their importance in carrying information that is vital to studies of the chemistry and evolution of star-forming regions, the collision rates of some of these molecules have not been available for rigorous studies in the past. Aims. Our goal is to perform an up-to-date gas and dust chemical characterization of two different star-forming regions, TMC 1-C and NGC 1333-C7, using new collisional rates of HCN, HNC, and their isotopologues. We investigated the possible effects of the environment and stellar feedback in their chemistry and their evolution. Methods. We used updated collisional rates of HCN, HNC, and their isotopologues in our analysis of the chemistry of TMC 1-C (Taurus) and NGC 1333-C7 (Perseus). With millimeter observations, we derived their column densities, the C and N isotopic fractions, the isomeric ratios, and the deuterium fractionation. The continuum data at 3 mm and 850 µm allowed us to compute the emissivity spectral index and look for grain growth as an evolutionary tracer. Results. The H13CN/HN13C ratio is anticorrelated with the deuterium fraction of HCN, thus it can readily serve as a proxy for the temperature. The spectral index (β ~ 1.34–2.09) shows a tentative anticorrelation with the H13CN/HN13C ratio, suggesting grain growth in the evolved, hotter, and less deuterated sources. Unlike TMC 1-C, the south-to-north gradient in dust temperature and spectral index observed in NGC 1333-C7 suggests feedback from the main NGC 1333 cloud. Conclusions. With this up-to-date characterization of two star-forming regions, we found that the chemistry and the physical properties are tightly related. The dust temperature, deuterium fraction, and the spectral index are complementary evolutionary tracers. The large-scale environmental factors may dominate the chemistry and evolution in clustered star-forming regions.

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Infrared Spectra of Acetylene Diluted in Solid Nitrogen Upon Irradiation With Vacuum Ultraviolet Light and Electrons

Cited by 13 publications

References 44 publications

Photoisomerization and Infrared Spectra of Allene and Propyne Cations in Solid Argon

Photoisomerization and Infrared Spectra of Allene and Propyne Cations in Solid Argon

Photochemistry and Astrochemistry: Photochemical Pathways to Interstellar Complex Organic Molecules

Linking the dust and chemical evolution: Taurus and Perseus

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