Evolution of planetary systeme

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Table of contents

1 Introduction: the search for exoplanets around low-mass stars 
1.1 A brief introduction of star-planet formation and evolution
1.1.1 Zoology of low-mass stars through the HR diagram
1.1.2 The formation of low-mass stars
1.1.2.1 Molecular clouds
1.1.2.2 The protostellar phase
1.1.2.3 Pre-main sequence phase
1.1.3 Planet formation around low-mass stars
1.1.3.1 Structure and properties of protoplanetary disks
1.1.3.2 The different steps of planet formation
1.1.4 Evolution of planetary systems
1.2 Current status of the search for exoplanets from Doppler and transit surveys
1.2.1 A brief overview of exoplanet detection techniques
1.2.2 Doppler spectroscopy
1.2.2.1 General principle
1.2.2.2 High-precision RV measurement
1.2.2.3 Brief history of the field and perspectives
1.2.3 Transiting planets
1.2.4 The diversity of exoplanetary worlds
1.2.5 The quest for habitable planets
1.3 The search for planets around M dwarfs and low-mass PMS stars
1.3.1 The case of very-low-mass stars
1.3.2 The case of low-mass PMS stars
1.4 Stellar activity and its impact on RV curves
1.4.1 Dynamo processes, stellar activity
1.4.1.1 Activity and rotation of low-mass stars
1.4.1.2 Surface inhomogeneities
1.4.1.3 Magnetic fields
1.4.1.4 Other sources of stellar activity RV signals
1.4.2 Modeling and filtering techniques
1.5 Observing M dwarfs and young stars with nIR velocimeters
1.5.1 SPIRou: un spectropolarimètre infrarouge
1.5.2 The SPIRou legacy survey and science goals
1.5.3 The challenges of nIR spectroscopy
1.6 Overview of the Ph.D. Thesis
2 Simulating nIR RV observations of low-mass stars with transiting planets 
2.1 Motivation and strategy
2.1.1 Motivation
2.1.2 TRAPPIST-1
2.1.3 K2-33
2.1.4 AU Mic
2.2 Method
2.2.1 Generating realistic stellar activity RV signals
2.2.1.1 Modelling the stellar surface with ZDI
2.2.1.2 Generating realistic densely-sampled stellar activity RV curves
2.2.1.3 Measuring the statistical properties of light-curves
2.2.1.4 Application to TRAPPIST-1, K2-33 and AU Mic
2.2.2 Building mock RV time-series
2.2.2.1 Planetary signals
2.2.3 Modeling the mock RV time-series
2.2.3.1 Quantifying the significance of each planet RV signature
2.3 Results and perspectives
2.3.1 Results for TRAPPIST-1
2.3.2 K2-33
2.3.3 Application to AU Microscopii
3 Modelling the magnetic field and activity of low-mass MS and PMS stars 
3.1 Context: magnetic field and activity of low-mass stars
3.1.1 Measuring magnetic fields
3.1.1.1 The Zeeman effect
3.1.1.2 Measuring magnetic fields from unpolarized spectra
3.1.1.3 Measuring polarized Zeeman signatures
3.1.2 Magnetic fields of M dwarfs and low-mass PMS stars
3.1.3 Magnetic interactions between stars and close-in planets
3.1.4 Modeling stellar activity to improve the filtering of the RV jitter
3.2 Spectropolarimetric analysis of low-mass stars
3.2.1 Spectropolarimetric measurements and data reduction
3.2.2 Mapping brightness inhomogeneities at the surface of low-mass stars with Doppler Imaging
3.2.3 Reconstructing large-scale magnetic topologies of low-mass stars with ZDI
3.2.4 Proxies for magnetic activity
3.3 Application to a sample of low-mass stars
3.3.1 AU Microscopii
3.3.2 Proxima Centauri
3.3.3 EPIC 211889233
3.3.4 V471 Tau
4 Measuring the mass of AU Mic b with SPIRou 
4.1 A Neptune-sized close-in planet around the PMS star AU Microscopii
4.2 Unveiling AU Mic b signature from SPIRou RV time-series
4.2.1 RV measurement process
4.2.2 RV modeling
4.2.3 Detection of the planet
4.2.4 Filtering stellar activity RV signal with ancillary indicators
4.3 Unveiling planet signature using ZDI
4.3.1 3D paraboloid fit
4.3.2 Using ZDI brightness map to filter stellar activity RV signals
4.4 Implications and perspectives
5 Probing the atmosphere of transiting planets around low-mass stars with SPIRou
5.1 Characterizing planet atmospheres
5.1.1 Structure and dynamics of exoplanetary atmospheres
5.1.2 Transit spectroscopy
5.1.3 Probing planet atmospheres with high-resolution spectroscopy
5.2 Unveiling planet atmospheres with SPIRou
5.2.1 Observations and description of the target
5.2.2 Pre-processing the sequences of spectra
5.2.2.1 Step 1: Preliminary cleaning
5.2.2.2 Step 2: Normalizing the spectra
5.2.2.3 Step 3: Detrending with airmass
5.2.2.4 Step 4: Outlier removal
5.2.2.5 Step 5: Correcting residuals with principal component analysis
5.2.3 Modeling the transmission spectrum of an exoplanet’s atmosphere
5.2.4 Correlation analysis
5.2.5 Validation on synthetic data
5.2.6 Preliminary results
5.2.7 Next steps for HD 189733 b and perspectives of improvement
5.3 Future prospects
5.3.1 The ATMOSPHERIX observation program
5.3.2 Transmission spectroscopy of AU Microscopii with SPIRou
6 Conclusions and perspectives