Abstract
The laboratory techniques, which have been applied to the determination of positive-ion/electron dissociation recombination coefficients, qe, and positive-ion/negative-ion mutual neutralization coefficients, qi, are briefly discussed. These include the stationary afterglow (SA), the variable-temperature flowing afterglow/Langmuir probe VT-FALP) and the merged beam (MB) techniques. It is suggested that the data of choice for interstellar ion-chemical models are those obtained using the truly thermal afterglow techniques rather than the qe deduced from cross section data obtained using the MB technique. A detailed discussion is presented of the various determinations of qe for H +3 ions which is now known to be very small. Some recent values of qe determined using the VT-FALP technique are given for positive ions of interstellar interest and, from the limited amount of data available concerning the temperature dependence of qe, appropriate values of qe for use in interstellar ion chemical models are suggested. Also briefly discussed are the most reliable values available for qi. These are included in view of the recent suggestion that significant concentrations of negatively-charged polycyclic aromatic hydrocarbons may exist in dense interstellar clouds and could undergo mutual neutralization reactions with ambient positive ions.
Keywords
- Proton Affinity
- Mutual Neutralization
- Interstellar Cloud
- Dissociative Recombination
- Recombination Coefficient
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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Adams, N.G., Smith, D. (1988). Laboratory Studies of Dissociative Recombination and Mutual Neutralization and Their Relevance to Interstellar Chemistry. In: Millar, T.J., Williams, D.A. (eds) Rate Coefficients in Astrochemistry. Astrophysics and Space Science Library, vol 146. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3007-0_11
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