Influence of cosmic rays

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Table of contents

I Context: CR irradiated molecular clouds 
1 The interstellar medium (ISM)
1.1 Structure of the ISM
1.2 Classification of gas clouds
1.3 Dense molecular clouds
1.4 ISM-star cycle
2 Cosmic rays
2.1 Discovery
2.2 Observations
2.3 Influence of cosmic rays
3 Cosmic-ray induced chemistry
3.1 The cosmic-ray ionisation rate
3.2 Diffuse molecular clouds
3.3 Dense molecular clouds
3.4 Propagation of the cosmic-ray spectrum
4 Interaction of supernova remnants with molecular clouds
4.1 Supernova remnants
4.2 Physical processes associated with gamma-ray emission
4.3 Evidence of the SNR interaction with molecular clouds
5 Thesis work: targets and methods 43
5.1 Open questions addressed by the thesis
5.2 Methods
5.3 Selection of the studied regions
II Methods: Radio observations and chemical modeling 
6 Observations
6.1 Radio astronomy
6.2 Molecular spectroscopy
6.3 IRAM 30m observations
7 Derivation of the column densities
7.1 Methodology
7.2 Data reduction
7.3 Derivation of physical conditions
7.4 Derivation of column densities
8 Chemical modeling
8.1 Chemical models
8.2 The astrochem code
8.3 Steady-state abundances
8.4 Comparison to observations
III Results 
9 Enhanced ionisation in W28 and CR properties
9.1 Introduction
9.2 Summary of the article and main results
9.3 Further considerations
10 Probing the passage of the W51C supernova remnant shock through a molecular cloud
10.1 Introduction
10.2 IRAM 30m observations
10.3 Dumas et al. 2014
11 New tracers of the ionisation
11.1 Introduction
11.2 Model predictions
11.3 Observations and results
11.4 Discussion
12 The W44 SNR-cloud association
12.1 Introduction
12.2 W44: Source background and strategy of observations
12.3 Observations and results
12.4 Analysis
12.5 Chemical modeling
12.6 Conclusions
13 Summary of the results and limits of the method
13.1 Summary of the results
13.2 Limitations of the method
Summary and perspectives
Résumé et perspectives
Bibliography 
Slides of the PhD defense