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Table of contents
1 Introduction
1.1 Star evolution
1.1.1 Interstellar gas
1.1.2 Interstellar dust
1.1.3 Surface chemistry
1.1.4 Interstellar molecules
1.1.5 Interstellar ices
1.2 Interaction of gas and grains
1.2.1 Gas phase
1.2.2 Solid phase sublimation
2 Experimental apparatus and Methods
2.1 Experimental apparatus
2.1.1 The main chamber
2.1.2 The sample holder and cryostat system
2.1.3 The beamline system
2.1.4 Quadrupole Mass Spectrometer (QMS)
2.1.5 The infrared spectroscopy
2.2 Experimental methods
2.2.1 Mass spectroscopy
2.2.1.1 Cracking pattern
2.2.1.2 Thermal Programmed Desorption (TPD)
2.2.2 Water ice substrates on the sample holder
2.2.3 Calibration of the beamline system
2.2.3.1 Optimization of the injection flow
2.2.3.2 Determination of the geometrical area of the beam deposition zone on the sample holder
2.2.3.3 Determination of the beam overlap
2.2.3.4 Dissociation of H2 and D2 beam
3 Segregation effect and N2 binding energy reduction in CO-N2 system adsorbed on water ice substrates
3.1 Introduction
3.2 Experimental protocol
3.3 Experimental results
3.3.1 Pure species
3.3.2 Mixed species
3.4 Analysis and discussion
3.5 Conclusions
4 Experimental study of the chemical network of the hydrogenation of NO on interstellar dust grains
4.1 Introduction
4.2 Experimental setup
4.3 Experimental results
4.3.1 Completeness of the reactions of the {NO + H} system before the TPD
4.3.2 Temperature dependency
4.3.3 The {NO + D} reactive system at various temperatures
4.4 Catalytic role of water
4.5 The possibility of back reaction NH2OH+H −! H2NO+H2
4.6 Experimental conclusions
4.7 Astrophysical implications
5 Study of the penetration of oxygen and deuterium atoms into porous water ice
5.1 Introduction
5.2 Experimental methods
5.2.1 Experimental set-up
5.2.2 Water ice characterization
5.3 Experimental results
5.3.1 Oxygenation of NO ices
5.3.2 Deuteration of NO ices
5.4 Model and Discussion
5.5 Astrophysical implications and conclusions
6 Efficient formation route of the pre-biotic molecule formamide on interstellar dust grains
6.1 Introduction
6.2 Experimental methods
6.3 Experimental results
6.4 Astrophysical implications
7 Experimental study of the hydrogenation of Acetonitrile and Methyl Isocyanide on Interstellar dust grains
7.1 Introduction
7.2 Experimental conditions
7.3 Experimental results
7.3.1 (Non) Reaction between Acetonitrile (CH3CN) and H atoms at 10 K
7.3.2 Reactivity between Methyl Isocyanide CH3NC and H atoms at 10 K
7.3.3 CH3NC and its hydrogenation in presence of H2O.
7.3.3.1 Desorption of CH3NC mixed with H2O
7.3.3.2 Reaction of CH3NC and H atoms in the presence of H2O
7.3.4 Reactivity of CH3NC and D atoms on the golden surface at 10 K
7.3.5 Reactivity of CH3NC and H atoms at various temperatures
7.4 Analysis and Discussion
7.4.1 Activation barrier and quantum tunneling
7.4.2 The catalytic role of H2O for chemical reactions
7.4.3 Orientation of CH3NC at different surface temperatures
7.4.4 Astrophysical implications
7.4.5 New estimation of the cracking patterns and of the binding energy of CH3NCH2
7.5 Summary and conclusion
8 Conclusions and perspectives
8.1 Remarks and Astrophysical implications
8.2 Perspectives
