Infrared spectra of triacetylene in the 4000-220 cm−1 region: Absolute band intensity and implications for the atmosphere of Titan

Delpech, C.; Guillemin, Jean‐Claude; Paillous, P.; Khlifi, M.; Bruston, P.; Raulin, F.

doi:10.1016/0584-8539(94)80031-6

Cited by 27 publications

(8 citation statements)

References 13 publications

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“…The remaining band at 1220 cm −1 cannot be attributed to a fundamental mode, since theoretical calculations do not forecast any mode close to this value. Previous work on triacetylene (17,(21)(22)(23)(24)(25) allows its identification as a very intense combination band, involving π g and π u modes. The combination π g π u produces the sum (26), where the term According to DFT calculations (Table 1), the other fundamental IR-active modes have an intensity 100 times weaker than the two stronger modes.…”

Section: Resultsmentioning

confidence: 99%

See 1 more Smart Citation

IR Spectrum of C8H2: Integrated Band Intensities and Some Observational Implications

Shindo

Bénilan

Chaquin

et al. 2001

Journal of Molecular Spectroscopy

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Section: Resultsmentioning

confidence: 99%

“…After the studies of diacetylene and triacetylene in our laboratory (17,18), we report here the first spectrum of gaseous tetraacetylene in the infrared range (400 cm −1 -4000 cm −1 ) and the integrated intensities obtained for the main bands. In the first section, the organic synthesis of C 8 H 2 is briefly described.…”

Section: Introductionmentioning

confidence: 99%

IR Spectrum of C8H2: Integrated Band Intensities and Some Observational Implications

Shindo

Bénilan

Chaquin

et al. 2001

Journal of Molecular Spectroscopy

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“…We estimate that we would have detected any feature at 16.1 µm amounting to 20% of the C 4 H 2 feature. Using a band strength of 312 cm −2 atm −1 (Delpech et al 1994), we derive an upper limit for the C 6 H 2 column density of 3 × 10 13 molecules cm −2 . This is an order of magnitude larger than predicted by the photochemical model.…”

Section: Table V Constraints From Iso Spectramentioning

confidence: 99%

Photochemistry of Saturn's Atmosphere I. Hydrocarbon Chemistry and Comparisons with ISO Observations

Moses

Bézard

Lellouch

et al. 2000

Icarus

284

326

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“…3.0×10 −7 Molecules that cannot be detected (proton affinity lower than H Delpech (1994) Due to the unit mass resolution of the instrument, most peaks cannot be uniquely identified based on mass alone. However, the requirement for the molecule to have a higher proton affinity than water eliminates a number of possibilities at the lower masses allowing for some unique identifications.…”

Section: Comparison To Titan's Atmospheric Compositionmentioning

confidence: 99%

Laboratory investigations of Titan haze formation: In situ measurement of gas and particle composition

Hörst

Yoon

Ugelow

et al. 2018

Icarus

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Prior to the arrival of the Cassini-Huygens spacecraft, aerosol production in Titan's atmosphere was believed to begin in the stratosphere where chemical processes are predominantly initiated by far ultraviolet (FUV) radiation. However, measurements taken by the Cassini Ultraviolet Imaging Spectrograph (UVIS) and Cassini Plasma Spectrometer (CAPS) indicate that haze formation initiates in the thermosphere where there is a greater flux of extreme ultraviolet (EUV) photons and energetic particles available to initiate chemical reactions, including the destruction of N 2 . The discovery of previously unpredicted nitrogen species in measurements of Titan's atmosphere by the Cassini Ion and Neutral Mass Spectrometer (INMS) indicates that nitrogen participates in the chemistry to a much greater extent than was appreciated before Cassini. The degree of nitrogen incorporation in the haze particles is important for understanding the diversity of molecules that may be present in Titan's atmosphere and on its surface. We have conducted a series of Titan atmosphere simulation experiments using either spark discharge (Tesla coil) or FUV photons (deuterium lamp) to initiate chemistry in CH 4 /N 2 gas mixtures ranging from 0.01% CH 4 /99.99% N 2 to 10% CH 4 /90% * sarah. N 2 . We obtained in situ real-time measurements using a high-resolution timeof-flight aerosol mass spectrometer (HR-ToF-AMS) to measure the particle composition as a function of particle size and a proton-transfer ion-trap mass spectrometer (PIT-MS) to measure the composition of gas phase products. These two techniques allow us to investigate the effect of energy source and initial CH 4 concentration on the degree of nitrogen incorporation in both the gas and solid phase products. The results presented here confirm that FUV photons produce not only solid phase nitrogen bearing products but also gas phase nitrogen species. We find that in both the gas and solid phase, nitrogen is found in nitriles rather than amines and that both the gas phase and solid phase products are composed primarily of molecules with a low degree of aromaticity. The UV experiments reproduce the absolute abundances measured in Titan's stratosphere for a number of gas phase species including C 4 H 2 , C 6 H 6 , HCN, CH 3 CN, HC 3 N, and C 2 H 5 CN.

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Infrared spectra of triacetylene in the 4000-220 cm−1 region: Absolute band intensity and implications for the atmosphere of Titan

Cited by 27 publications

References 13 publications

IR Spectrum of C8H2: Integrated Band Intensities and Some Observational Implications

IR Spectrum of C8H2: Integrated Band Intensities and Some Observational Implications

Photochemistry of Saturn's Atmosphere I. Hydrocarbon Chemistry and Comparisons with ISO Observations

Laboratory investigations of Titan haze formation: In situ measurement of gas and particle composition

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