<b>Reaction of Methylene Radicals with Acetylene in the Gas Phase</b>

Terao, Terumi; Sakai, Nobuyoshi.; Shida, Shôji

doi:10.1021/ja00907a002

Cited by 18 publications

(8 citation statements)

References 3 publications

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“…At room temperature, in the two-body limit, Laufer and Bass (1974) obtained k 31 = k 31 a + k 31 b = 7.5X10-12 cm 3 s-1 , a value which should be compared with 4.0x10-12 cm 3 s-1, as reported by Pilling and Robertson (1977). Laufer (198la) proposed an average value for k 31 =5.8±1.8X10-12 cm 3 s-1 • The ratio of the two channels k 31 a/k 31 b is 0.50 and 0.59, according to Laufer and Bass (1974) and Pilling and Robertson (1977), respectively, in marked contrast to the value 1.5 re-ported by Terao, Sakai, and Shida (1963). The difference could be attributed to the presence of 1 CH 2 in the experiment by Terao et al (Laufer 198la).…”

Section: A) Dissociationmentioning

confidence: 76%

Photochemistry of the atmosphere of Titan - Comparison between model and observations

Yung¹,

Allen²,

Pinto³

1984

ApJS

975

614

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The photochemistry of simple molecules containing carbon, hydrogen, nitrogen, and oxygen atoms in the atmosphere of Titan has been investigated using updated chemical schemes and our own estimates of a number of key rate coefficients. Proper exospheric boundary conditions, vertical transport, and condensation processes at the tropopause have been incorporated into the model. It is argued that he composition, climatology, and evolution of Titan's atmosphere are controlled by five major processes: (a) photolysis and photosensitized dissociation of CH4; (b) conversion of H to H2 and escape of hydrogen; (c) synthesis of higher hydrocarbons; (d) coupling between nitrogen and hydrocarbons; (e) coupling between oxygen and hydrocarbons. Starting with N2, CH4, and H2O, and invoking interactions with ultraviolet sunlight, energetic electrons, and cosmic rays, the model satisfactorily accounts for the concentrations of minor species observed by the Voyager IRIS and UVS instruments. Photochemistry is responsible for converting the simpler atmospheric species into more complex organic compounds, which are subsequently condensed at the tropopause and deposited on the surface. Titan might have lost 5.6 x 10(4), 1.8 x 10(3), and 4.0 g cm-2, or the equivalent of 8, 0.25, and 5 x 10(-4) bars of CH4, N2, and CO, respectively, over geologic time. Implications of abiotic organic synthesis on Titan for the origin of life on Earth are briefly discussed.

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Section: A) Dissociationmentioning

confidence: 76%

Photochemistry of the atmosphere of Titan - Comparison between model and observations

Yung¹,

Allen²,

Pinto³

1984

ApJS

975

614

View full text Add to dashboard Cite

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“…13 the main reaction routes to the hydrocarbons C,H4 and C4H, as well as to CO and H atoms are indicated by heavy arrows. Of the other reactions some do only play a role if one reactant is present in a large excess (reactions (15) and (21) for large [C2H2],, reactions (2), (22), (23), and (14) for an excess of [HI,). The reactions consuming C3H4 and C4H2 have to be included, particularly those for C4H2.…”

Section: The Mechanism Used For Calculationsmentioning

confidence: 99%

Kinetics and Mechanism of Hydrocarbon Formation in the System C₂H₂/H

Homann

Schweinfurth

1981

Ber Bunsenges Phys Chem

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The formation of C3H4 (Propyne and Allene), C4H2 (Butadiyne) and also of formaldehyde in the system C 2 H 2 / 0 with and without added H atoms was studied at 298 K and in a pressure range between 1.4 and 8.0 mbar. H atoms have a strongly positive influence on the rates of formation of these species. The results obtained for largely varying initial conditions were described quantitatively by a reaction mechanism of 25 reactions.Experiments with D atoms and with different 0, concentrations gave additional evidence of the radical reactions involved.

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“…Final products of the reaction lCH z + CzH z have been analysed by several authors at total pressures of p~3 bar [11][12][13][14]. They report that methylacetylene and allene arise as main products with branching ratios klOa/k lOb = 1.0-1.5…”

Section: Discussionmentioning

confidence: 99%

Direct Determination of CH₂(ã¹A₁) Removal Rates by C₂H₂ and C₆H₆

Hack

Koch

Wagner

et al. 1988

Ber Bunsenges Phys Chem

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Gas phase reactions of CH2(ã1A1) with benzene C6H6 and acetylene C2H2 were investigated at room temperature. CH2(ã1A1) was generated by laser photolysis of CH2CO at λL = 308 nm and the reactions were monitored directly by measuring the removal of CH2(ã1A1) with laser‐induced fluorescence (LIF). For the measurement of the formation rate of 3CH2 by physical deactivation LMR detection was used. The total removal of CH2(ã1A1) was found to be very efficient with rate constants of 2.4 ± 0.5 and 2.2 ± 0.2 (in 1014 cm3/mol s) for C6H6 and C2H2, respectively. The physical deactivation of 1CH2 to 3CH2 is about 30 resp. 22 percent of the total removal rate. Activation rates of 3CH2 to 1CH2 are give

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Reaction of Methylene Radicals with Acetylene in the Gas Phase

Cited by 18 publications

References 3 publications

Photochemistry of the atmosphere of Titan - Comparison between model and observations

Photochemistry of the atmosphere of Titan - Comparison between model and observations

Kinetics and Mechanism of Hydrocarbon Formation in the System C₂H₂/H

Direct Determination of CH₂(ã¹A₁) Removal Rates by C₂H₂ and C₆H₆

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Reaction of Methylene Radicals with Acetylene in the Gas Phase

Cited by 18 publications

References 3 publications

Photochemistry of the atmosphere of Titan - Comparison between model and observations

Photochemistry of the atmosphere of Titan - Comparison between model and observations

Kinetics and Mechanism of Hydrocarbon Formation in the System C2H2/H

Direct Determination of CH2(ã1A1) Removal Rates by C2H2 and C6H6

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Product

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Kinetics and Mechanism of Hydrocarbon Formation in the System C₂H₂/H

Direct Determination of CH₂(ã¹A₁) Removal Rates by C₂H₂ and C₆H₆