ChemInform Abstract: Formation of HCN and Acetylene Oligomers by Photolysis of Ammonia in the Presence of Acetylene: Applications to the Atmospheric Chemistry of Jupiter.

Ferris, James P.; Ishikawa, Yoji

doi:10.1002/chin.198842118

Cited by 4 publications

(4 citation statements)

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“…Many experimental techniques have been developed to simulate the formation of organics from the coupling of the chemistry of CH4 and the resulting higher hydrocarbons (mainly C2H2)and NH 3 in a mode! Jovian atmosphere using UV radiation [Bossard and Toupance, 1980;Raulin et al, 1979;Ferris and Ishikawa, 1988;Ferris et al, 1992), and electric discharges [Sagan and Miller, 1960;Ponnarnperuma et al, 1969;Stribling and Miller, 1987;McDonald et al, 1992]. These experiments predict, in particular, that C 2 hydrocarbons, HCN and benzene should be present in noticeable amounts in the atmosphere of Jupiter and indeed they all have been detected [Ridgway et al, 1974, Tokunaga et al, 1981, K#n et al, 1985.…”

Section: Simulation Experimentsmentioning

confidence: 99%

Laboratory studies of organic chemistry in planetary atmopheres: From simulation experiments to spectroscopic determinations

Bruston¹,

Khlifi²,

Bénilan³

et al. 1994

J. Geophys. Res.

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Possible approaches to the study of organic chemistry in planetary atmospheres are threefold: they comprise theoretical modeling, simulation experiments, and observational programs. Because of their respective merits and limitations, these approaches are quite complementary, and their simultaneous improvement is the way to progress further in the field. All three ask for laboratory work, and the lack, or limited accuracy, of laboratory data is the main restriction to future improvement. Together with the development of theoretical modeling (based on chemical kinetics and depending on laboratory studies of reaction pathways and rate constants) laboratory simulation remains a powerful technique. Despite the inaccurate reproduction of all planetary conditions, this experimental approach yields precious information on the nature of middle and higher order molecular weight organics that can be expected in an atmosphere of a given overall composition; and there is, in general, good agreement between the data obtained from simulations and those derived from observations. Indeed, several of the organic species highlighted in such experiments, and their relative abundances, are compatible with those detected in related planetary atmospheres. This is shown in the particular case of Titan. Thus experimental results furnish information on the nature of organics to be searched for in planetary atmospheres, while, in turn, the detection of such candidates and possible indications of their concentration profiles, or the setting of upper limits to their abundancies, constrain the kinetic approach. Given the lists of candidates from simulation experiments, experimental programs for a systematic determination of spectroscopic characteristics, including frequencies and band or line intensities, of the likely organics in planetary atmospheres, have to be developed. As an example, experimental requirements and current results, both in the IR and the UV range, are presented concerning Titan's atmosphere in view of the Cassini‐Huygens mission.

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Section: Simulation Experimentsmentioning

confidence: 99%

Laboratory studies of organic chemistry in planetary atmopheres: From simulation experiments to spectroscopic determinations

Bruston¹,

Khlifi²,

Bénilan³

et al. 1994

J. Geophys. Res.

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“…These processes eventually result in the production of polyacetylenes or polyynes which are candidates for jovian aerosols (West et al, 1986). Furthermore, the coupled photochemistry of acetylene with ammonia (NH 3 ) has been postulated (Kaye and Strobel, 1983) and verified in the laboratory (Ferris and Ishikawa, 1988) to lead to the formation of hydrogen cyanide (HCN).…”

Section: Introductionmentioning

confidence: 99%

HST observation of the atmospheric composition of Jupiter’s equatorial region: evidence for tropospheric C2H2☆

Bétrémieux

Yelle

Griffith

2003

Icarus

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This paper presents the first detailed analysis of acetylene absorption features observed longward of 190.0 nm in a jovian spectrum by the Faint Object Spectrograph on board the Hubble Space Telescope. The presence of two features located near 207.0 nm can only be explained by a substantial abundance of acetylene in the upper troposphere. Using a Rayleigh-Raman radiative transfer model, it was determined that the acetylene vertical profile is characterized by a decrease in the mole fraction with increasing pressure in the upper stratosphere, a minimum around 14 to 29 mbar, followed by an increase to about 1.5 ϫ 10 Ϫ7 in the upper troposphere. Longward of 220 nm, the relatively high contrast of Raman features to the continuum precludes the existence of an optically significant amount of clouds from 150 to 500 mbar unless they are highly reflective. Instead, the reflectivity at these long wavelengths is determined by stratospheric, not tropospheric, scatterers and absorbers. Analysis of the data also suggests that ammonia is extremely undersaturated at pressures below 700 mbar. However, no firm conclusions can be reached because of the uncertainties surrounding its cross section longward of 217.0 nm, which are due to vibrationally excited states.

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“…CH3CN is detected in comets (Donn, 1982), the interstellar medium (Mann and Williams, 1980) and is formed in FIT reactions from CO, NH3 and H2 (Hayatsu et al, 1968(Hayatsu et al, , 1972, by the photolysis of mixtures of acetylene and NH3 (Ferris and Ishikawa, 1988) and the photolysis of acetamide (CH3CONH2) (Spall and Steacie, 1957). No studies suggest that CH3CN has a role in prebiotic synthesis so its presence is not indicative of processes leading to the origins of life but it may be formed in hydrothermal systems.…”

Section: Acetonitrile (Ch3cn)mentioning

confidence: 95%

Marine Hydrothermal Systems and the Origin of Life

Holm¹

1992

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ChemInform Abstract: Formation of HCN and Acetylene Oligomers by Photolysis of Ammonia in the Presence of Acetylene: Applications to the Atmospheric Chemistry of Jupiter.

Cited by 4 publications

References 1 publication

Laboratory studies of organic chemistry in planetary atmopheres: From simulation experiments to spectroscopic determinations

Laboratory studies of organic chemistry in planetary atmopheres: From simulation experiments to spectroscopic determinations

HST observation of the atmospheric composition of Jupiter’s equatorial region: evidence for tropospheric C2H2☆

Marine Hydrothermal Systems and the Origin of Life

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