Gas-phase heteroaromatic substitutions. 5. Gas-phase protonation of five-membered heteroaromatic rings by hydro-t-helium(1+)-3He (3HeT+) ions. A model reaction for a theoretical approach to heteroaromatic reactivity

1984 ◽  
Vol 106 (1) ◽  
pp. 37-41 ◽  
Author(s):  
Giancarlo Angelini ◽  
Giuseppe Laguzzi ◽  
Cinzia Sparapani ◽  
Maurizio Speranza
Keyword(s):  
Gas Phase ◽  
Theoretical Approach ◽  
Model Reaction

scholarly journals Translucent Clouds as Testbeds of Basic Chemical Networks

2000 ◽  
Vol 197 ◽  
pp. 31-40
Author(s):  
B. E. Turner
Keyword(s):  
Standard Model ◽  
Gas Phase ◽  
Molecular Species ◽  
Model Reaction ◽  
Gas Phase Chemistry ◽  
Diffuse Cloud ◽  
Phase Chemistry

We have developed comprehensive models, based on the New Standard Model reaction dataset, for the gas-phase chemistry of translucent clouds. These models predict satisfactorily the abundances of 34 of the 38 molecular species observed in both translucent and cold dense clouds. With 3 additional reactions, the models also appear able to explain diffuse cloud abundances.

Mechanistic Insight into the Molecular TiO2-Mediated Gas Phase Detoxication of DMMP: A Theoretical Approach

2017 ◽  
Vol 30 (5) ◽  
pp. 1177-1187 ◽  
Author(s):  
Tamalika Ash ◽  
Tanay Debnath ◽  
Avik Ghosh ◽  
Abhijit Kumar Das
Keyword(s):  
Gas Phase ◽  
Theoretical Approach ◽  
Mechanistic Insight ◽  
Insight Into

scholarly journals Silicate, ruby, opal – Why gas giants keep their jewels in the atmosphere

2007 ◽  
Vol 3 (S249) ◽  
pp. 167-172
Author(s):  
Christiane Helling
Keyword(s):  
Gas Phase ◽  
Theoretical Approach ◽  
Homogeneous Nucleation ◽  
Strong Influence ◽  
Cloud Formation ◽  
Gravitational Settling ◽  
Dust Clouds ◽  
Synthetic Spectra ◽  
Dust Complex ◽  
First Time

AbstractGiant gas-planets - and brown dwarfs - form dust clouds in their atmospheres which are made of a variety of gemstone-like and possible liquid materials. Our theoretical approach, where we calculate homogeneous nucleation, heterogeneous growth/evaporation, gravitational settling, and element consumption for composite dust grains, allows to access the evolution of the dust complex in the cloud, and hence also the elements remaining in the gas phase. The cloud formation process is imprinted into these remaining elements. Following a (T, p) trajectory into the atmosphere we observe that 1. metals disappear, 2. dust forms, 3. metals re-appear, 4. dust disappears. For the first time, our kinetic cloud formation approach is coupled with an 1D atmosphere simulation and, hence, synthetic spectra can be produced based on detailed cloud micro-physics. Results are demonstrated for metal-poor gas giants and the strong influence of the dust modelling on alkali-line profile is shown.

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