Systematic Search for Chemical Reactions in Gas Phase Contributing to Methanol Formation in Interstellar Space

2017 ◽  
Vol 121 (39) ◽  
pp. 7393-7400 ◽  
Author(s):  
Victoria G. Gamez-Garcia ◽  
Annia Galano
Keyword(s):  
Gas Phase ◽  
Chemical Reactions ◽  
Systematic Search ◽  
Interstellar Space ◽  
Methanol Formation

Chemical reactions between cold trappedBa+ions and neutral molecules in the gas phase

2008 ◽  
Vol 78 (4) ◽  
Author(s):  
B. Roth ◽  
D. Offenberg ◽  
C. B. Zhang ◽  
S. Schiller
Keyword(s):  
Gas Phase ◽  
Chemical Reactions

scholarly journals Surface Reactions in Interstellar Space

2002 ◽  
Vol 12 ◽  
pp. 55-57 ◽  
Author(s):  
Eric Herbst
Keyword(s):  
Surface Chemistry ◽  
Gas Phase ◽  
Condensed Phase ◽  
Current Knowledge ◽  
Surface Reactions ◽  
Future Research ◽  
Interstellar Space ◽  
Interstellar Molecules ◽  
Grain Surface

AbstractIt is impossible to explain the abundances of some gas-phase and most condensed-phase interstellar molecules without the use of grain chemistry. Nevertheless, grain-surface chemistry is relatively poorly understood for a variety of reasons. Our current knowledge of this chemistry and its use in interstellar models is discussed along with specific needs for future research.

scholarly journals Nucleation and Grain Growth in Interstellar Space

1965 ◽  
Vol 7 ◽  
pp. 191-206
Author(s):  
Bertram Donn
Keyword(s):  
Grain Growth ◽  
Chemical Reactions ◽  
Low Temperatures ◽  
Stellar Atmospheres ◽  
Interstellar Space ◽  
Considerable Influence ◽  
Direct Bearing ◽  
Interstellar Grains ◽  
Made In

The First Detailed Studies to determine the processes by which interstellar grains may form were made by a group of Dutch astronomers in the 1940's. (See refs. 1 to 5.) Since that time very little systematic work on this problem has been done until very recently when Hoyle and Wickramasinghe (ref. 6) investigated graphite formation in cool stellar atmospheres. Van de Hulst's paper in 1949 (ref. 5) represents the culmination of an intensive attack which had considerable influence on astronomical thought about interstellar grains.Somewhat ironically, beginning about 1949 many significant advances in physics and chemistry having a direct bearing on this problem were made. In 1949, Frank in reference 7 presented a theory which explained how real crystals tend to grow, and much work, both theoretical and experimental, has been done since then. (See ref. 8.) Recent extensive research in chemical reactions at low temperatures both in solids and on surfaces is reported in reference 9.

The Role of Starting Potential in the Kinetics of Chemical Reactions under Electrodeless Discharge

1970 ◽  
Vol 25 (11) ◽  
pp. 1772
Author(s):  
T.S.R Ao ◽  
A. Patil
Keyword(s):  
Gas Phase ◽  
Chemical Reactions ◽  
Electric Discharge ◽  
Specific Rate ◽  
Gas Phase Reactions ◽  
Electrodeless Discharge ◽  
First Order ◽  
Kinetics Of

Abstract It has been shown that in kinetically first order gas phase reactions occuring under electric discharge, such as the decomposition of N2O, the application, at various initial pressures, of the same multiple of the respective starting potential ensures that the reaction occurs at the same specific rate.

scholarly journals Astrochemistry of Interstellar Clouds: II. Molecular Formation in a Contracting Cloud

1987 ◽  
Vol 120 ◽  
pp. 273-274
Author(s):  
M.A. El Shalaby ◽  
A. Aiad
Keyword(s):  
Gas Phase ◽  
Optical Depth ◽  
Chemical Reactions ◽  
Particle Density ◽  
Interstellar Cloud ◽  
Gas Phase Reactions ◽  
Interstellar Clouds ◽  
Continous Function ◽  
Molecular Formation ◽  
Self Gravity

The chemistry of an 667 Mo interstellar cloud was studied using 142 reactions for 40 species during the contraction under self gravity in two steps. At first the contraction is allowed without gas phase reactions untill certain optical depth is reached. Secondly, at this optical depth the chemical reactions are started for sufficient cycles in a time dependant scheme till only very small additionally changes in the abundances occur. The so obtained, relative abundances and coulmn densities for different species represent a continous function of the optical depths. The values arround τ=6.3 represent the observations for H2, H2+, H3+, OH, OH+, CH, CH+, CH2, CH2+, CH3+, H2O and H3O+. The region of τ between 1 and 5 i.e. of particle density between 4 102–6 103 is the preferable formation place for the majority of molecules.

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