Plasma-assisted ignition and combustion

Aims. We present a new version of the UMIST Database for Astrochemistry, the fourth such version to be released to the public. The current version contains some 4573 binary gas-phase reactions, an increase of 10% from the previous (1999) version, among 420 species, of which 23 are new to the database. Methods. Major updates have been made to ion-neutral reactions, neutral-neutral reactions, particularly at low temperature, and dissociative recombination reactions. We have included for the first time the interstellar chemistry of fluorine. In addition to the usual database, we have also released a reaction set in which the effects of dipole-enhanced ion-neutral rate coefficients are included. Results. These two reactions sets have been used in a dark cloud model and the results of these models are presented and discussed briefly. The database and associated software are available on the World Wide Web at www.udfa. net.

/pdf/the-umist-database-for-astrochemistry-2006-1zuqm22qmy.pdf

The UMIST Database for Astrochemistry 2006

A detailed global model of atmospheric-pressure He + H2O plasmas is presented in this paper. The model incorporates 46 species and 577 reactions. Based on simulation results obtained with this comprehensive model, the main species and reactions are identified, and simplified models capable of capturing the main physicochemical processes in He + H2O discharges are suggested. The accuracy of the simplified models is quantified and assessed for changes in water concentration, input power and electrode configuration. Simplified models can reduce the number of reactions by a factor of similar to 10 while providing results that are within a factor of two of the detailed model. The simulation results indicate that Penning processes are the main ionization mechanism in this kind of discharge (1-3000 ppm of water), and water clusters of growing size are found to be the dominant charged species when the water concentration is above similar to 100 ppm. Simulation results also predict a growing electronegative character of the discharge with increasing water concentration. The use of He + H2O discharges for the generation of reactive oxygen species of interest in biomedical applications and the green production of hydrogen peroxide are also discussed. Although it would be unrealistic to draw conclusions regarding the efficacy of these processes from a zero-dimensional global model, the results indicate the potential suitability of He + H2O plasmas for these two applications.

https://iopscience.iop.org/article/10.1088/0963-0252/19/2/025018/pdf

Global model of low-temperature atmospheric-pressure He + H2O plasmas

Observations of H{sup +}{sub 3} in the Galactic diffuse interstellar medium have led to various surprising results, including the conclusion that the cosmic-ray ionization rate ({zeta}{sub 2}) is about one order of magnitude larger than previously thought. The present survey expands the sample of diffuse cloud sight lines with H{sup +}{sub 3} observations to 50, with detections in 21 of those. Ionization rates inferred from these observations are in the range (1.7 {+-} 1.3) Multiplication-Sign 10{sup -16} s{sup -1} < {zeta}{sub 2} < (10.6 {+-} 8.2) Multiplication-Sign 10{sup -16} s{sup -1} with a mean value of {zeta}{sub 2} = (3.5{sup +5.3}{sub -3.0}) Multiplication-Sign 10{sup -16} s{sup -1}. Upper limits (3{sigma}) derived from non-detections of H{sup +}{sub 3} are as low as {zeta}{sub 2} < 0.4 Multiplication-Sign 10{sup -16} s{sup -1}. These low upper limits, in combination with the wide range of inferred cosmic-ray ionization rates, indicate variations in {zeta}{sub 2} between different diffuse cloud sight lines. A study of {zeta}{sub 2} versus N{sub H} (total hydrogen column density) shows that the two parameters are not correlated for diffuse molecular cloud sight lines, but that the ionization rate decreases when N{sub H} increases to values typical of dense molecular clouds. Bothmore » the difference in ionization rates between diffuse and dense clouds and the variation of {zeta}{sub 2} among diffuse cloud sight lines are likely the result of particle propagation effects. The lower ionization rate in dense clouds is due to the inability of low-energy (few MeV) protons to penetrate such regions, while the ionization rate in diffuse clouds is controlled by the proximity of the observed cloud to a site of particle acceleration.« less

https://iopscience.iop.org/article/10.1088/0004-637X/745/1/91/pdf

Investigating the cosmic-ray ionization rate in the galactic diffuse interstellar medium through observations of h+ 3

We present results from high-resolution three-dimensional simulations of turbulent interstellar gas that self-consistently follow its coupled thermal, chemical and dynamical evolution, with a particular focus on the formation and destruction of H 2 and CO. We quantify the formation time-scales for H 2 and CO in physical conditions corresponding to those found in nearby giant molecular clouds, and show that both species form rapidly, with chemical time-scales that are comparable to the dynamical time-scale of the gas. We also investigate the spatial distributions of H 2 and CO, and how they relate to the underlying gas distribution. We show that H 2 is a good tracer of the gas distribution, but that the relationship between CO abundance and gas density is more complex. The CO abundance is not well-correlated with either the gas number density n or the visual extinction Av : both have a large influence on the CO abundance, but the inhomogeneous nature of the density field produced by the turbulence means that n and A v are only poorly correlated. There is a large scatter in A v , and hence CO abundance, for gas with any particular density, and similarly a large scatter in density and CO abundance for gas with any particular visual extinction. This will have important consequences for the interpretation of the CO emission observed from real molecular clouds. Finally, we also examine the temperature structure of the simulated gas. We show that the molecular gas is not isothermal. Most of it has a temperature in the range of 10-20 K, but there is also a significant fraction of warmer gas, located in low-extinction regions where photoelectric heating remains effective.

A. Mitchell

Papers

The dissociative recombination of molecular ions