Reaktionen von Molekülen in definierten Schwingungszuständen (IV). Reaktionen schwingungsangeregter Cyan‐Radikale mit Wasserstoff und einfachen Kohlenwasserstoffen

Schacke, H.; Wagner, H. Gg.; Wolfrum, J.

doi:10.1002/bbpc.19770810709

Cited by 55 publications

(12 citation statements)

References 10 publications

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“…The kinetics for schemes (13)-(15) has been fairly well established by recent studies (Laufer 198lb;Okabe 1981;Schacke, Wagner, and Wolfrum 1977;Becker and Hong 1983).…”

Section: Net Chemical Reactionmentioning

confidence: 72%

“…x 10-31 Black et al 1969 Estimated, see text Mayer et al 1966Westley 1980 Estimated, see text Schacke et al 1977Estimated Schacke et al 1977Becker and Hong 1983 H 2 0 and C0 2 photochemistry, are well understood from our experience with the terrestrial planets. These subjects will not be further discussed.…”

Section: Referencementioning

confidence: 99%

“…The alternative pathway, abstraction of a hydrogen atom, most probably has a high activation energy. Some of the products in reactions (R80)-(R82) have been identified in experiments by Herron, Franklin, and Bradt (1959) and Schacke, Wagner, and Wolfrum (1977). The appropriate rate coefficients listed in Table 3C have been estimated using Schacke, Wagner, and Wolfrum (1977), Becker and Hong (1983), and analogy with similar reactions involving the ethynyl radical.…”

Section: A) Dissociationmentioning

confidence: 99%

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

Yung¹,

Allen²,

Pinto³

1984

ApJS

968

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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“…The kinetics for schemes (13)-(15) has been fairly well established by recent studies (Laufer 198lb;Okabe 1981;Schacke, Wagner, and Wolfrum 1977;Becker and Hong 1983).…”

Section: Net Chemical Reactionmentioning

confidence: 72%

Section: Referencementioning

confidence: 99%

Section: A) Dissociationmentioning

confidence: 99%

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

Yung¹,

Allen²,

Pinto³

1984

ApJS

968

614

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“…The only previous direct determination of k2 is due to Albers et al [3,4], who report the following expression: k2 = (6 f 2) X 1013 exp(-2670 f 300/T)cm3/mol -s in the temperature range of 295-388 K. …”

Section: Introductionmentioning

confidence: 99%

High‐temperature determination of the rate coefficient for the reaction H₂ + CN → H + HCN

Szekely

Hanson

Bowman

1983

Int J of Chemical Kinetics

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The rate coefficient of the reaction (2) Hz + CN + H + HCN has been determined in the temperature range of 2700-3500 K using a shock tube technique.CZNTHTAr mixtures were heated behind incident shock waves and the early-time CN history was monitored using broad-band absorption spectroscopy. The rate coefficient providing the best fit to the data was k = (7.5350) x 1013 crnVmo1-s in good agreement with extrapolations of previously published low-temperature results.

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“…2 The reaction of H + HCN f H 2 + CN is endothermic by 90 kJ/mol 1 and exhibits a total barrier of 112 ( 3 kJ/mol. 3 Ab initio calculations predict that both Cl + HCN f HCl + CN 4 and H + HCN f H 2 + CN 5 proceed via linear transition states. This is consistent with the experimental observations of rotationally low excited CN product molecules.…”

Section: Introductionmentioning

confidence: 99%

Stereocontrol of Reactive Encounters Using Polarized Light

1997

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The reaction geometry of selected species can be controlled by using polarized light even in bulk experiments. One reactant A is generated in a photodissociation process. Its spatial distribution is completely described by the anisotropy parameter β. The other molecular reactant B is excited in a specific rovibrational state. Its spatial distribution is given by the j-and branch-dependent alignment parameter A 0 (2) . The unnormalized probability of an attack of A on B under an angle γ is then given by the simple expression P(γ) ∝ [1 + 1 / 5 βA 0 (2) P 2 (cos γ) P 2 (cos δ)], where δ is the angle between the E B-vectors of the dissociating and of the exciting laser beams. P 2 (x) represents the second Legendre polynom. We have studied the reaction of X + HCN f HX + CN with X ) H, Cl. The attacking H atom is generated in the photodissociation of CH 3 SH at 266 nm, and the chlorine atom is formed in the photolysis of Cl 2 at 355 nm. In both cases the β-parameter is close to -1. In order to align the HCN partner reactant, the first and third vibrational overtone of the CH stretch vibration was excited via the R and P branches. The nascent CN(V)0) product molecules were observed by laser induced fluorescence (LIF). The experimental results prove a preferred linear reaction geometry, i.e. an end-on attack of the X atom on the terminating hydrogen atom of the HCN reactant. However, the angle of acceptance is higher for the Cl + HCN reaction than for the H + HCN one.

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Reaktionen von Molekülen in definierten Schwingungszuständen (IV). Reaktionen schwingungsangeregter Cyan‐Radikale mit Wasserstoff und einfachen Kohlenwasserstoffen

Cited by 55 publications

References 10 publications

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

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

High‐temperature determination of the rate coefficient for the reaction H₂ + CN → H + HCN

Stereocontrol of Reactive Encounters Using Polarized Light

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Reaktionen von Molekülen in definierten Schwingungszuständen (IV). Reaktionen schwingungsangeregter Cyan‐Radikale mit Wasserstoff und einfachen Kohlenwasserstoffen

Cited by 55 publications

References 10 publications

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

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

High‐temperature determination of the rate coefficient for the reaction H2 + CN → H + HCN

Stereocontrol of Reactive Encounters Using Polarized Light

Contact Info

Product

Resources

About

High‐temperature determination of the rate coefficient for the reaction H₂ + CN → H + HCN