The PIONIER Instrument

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Table of contents

1 Scientific overview 
1.1 Star formation
1.2 Protoplanetary disk phase
1.3 Planet formation
1.4 The radial structure of the disk
1.5 The vertical structure of the disk
1.6 Dust properties
1.6.1 Dust opacity
1.6.2 Dust scattering
1.6.3 Mie Theory
1.7 Protoplanetary disk Models
1.7.1 Transitional and Pre-transitional Disks
1.8 Radiative transfer
1.8.1 The radiative transfer problem
1.8.2 Monte Carlo radiative transfer: MCFOST
2 An introduction to optical/IR interferometry 
2.1 Why Spatial Interferometry?
2.1.1 The Electromagnetic field
2.1.2 The Young’s experiment
2.1.3 The Fizeau Interferometry
2.1.4 Light coherence
2.1.5 Complex degree of mutual coherence
2.1.6 Visibility
2.1.7 Phase
2.1.8 The differential phase
2.1.9 The closure phase
2.2 Interferometric facilities around the world
2.2.1 The VEGA Instrument
2.2.2 The PIONIER Instrument
2.2.3 The MIDI Instrument
3 The peculiar fast-rotating star 51 Oph probed by VEGA/CHARA 
3.1 Abstract
3.2 Introduction
3.3 Observations and data processing
3.4 Continuum emission: stellar photosphere
3.5 Hα emission line
3.5.1 Qualitative analysis
3.5.2 Kinematic model
3.6 Discussions
4 Probing the inner region of the pre-transitional disk of HD 100546 
4.1 Abstract
4.2 Introduction
4.3 Observations
4.4 Data description
4.4.1 Visibilities
4.4.2 Closure phase
4.4.3 The spectral energy distribution
4.5 Modeling
4.5.1 The radiative transfer code
4.5.2 Methodology
4.5.3 Evaluation of sensitivity to parameters
4.5.4 Results
4.6 Do we have evidence for a clumpy structure?
4.7 Conclusion
5 Study of the inner disk of the Herbig star MWC 480 
5.1 Abstract
5.2 Introduction
5.3 Observations
5.3.1 MIDI observations and data reduction
5.3.2 Spectroscopic observations
5.3.2.1 Variability
5.4 Modeling
5.4.1 Application to the one-component disk model
5.4.1.1 Results
5.4.2 Application to the two-component disk model
5.4.2.1 Results
5.5 Summary and perspectives
6 The possible asymmetrical models for explaining the inner disk struc- ture of MWC480 
6.1 Abstract
6.2 Introduction
6.3 Observations
6.3.1 MIDI observations
6.3.2 Spectroscopic observations with SpeX
6.4 Modeling
6.4.1 Azimuthally asymmetric models
6.4.1.1 Two-component disk model with wall
6.4.1.2 A two-component disk model with a bright feature
6.5 Discussion
6.6 Summary and perspectives
7 Conclusion and future work 
7.1 The visible point of view
7.2 The near- and mid-Infrared point of view
7.3 Conclusions
7.4 Future investigations
Bibliography