Thesis
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Thesis
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1 - Introduction
1.1. The structure of the Sun
1.2. The solar wind
1.3. A brief history of the discovery of the solar wind
Chromosphere
Convection zone
Core of the Sun
Corona
Coronal heating problem
Interaction of the solar wind with the Earth's magnetosphere
Magnetosheath
Models of the solar corona
Photosphere
Proton-proton cycle
Radiation zone
Transition region
2 - Basic concepts in hydrodynamic and magnetohydrodynamic turbulence
2.1. Reynolds decomposition
2.2. Correlation function
2.4. Kolmogorov's theory of turbulence
2.5. Iroshnikov-Kraichnan spectrum
2.5. Taylor hypothesis
Structure function
3 - Basic concepts in plasma physics and magnetohydrodynamics
Boltzmann equation
Important timescales
MHD equations
Moments of the Vlasov equation
4 - von Karman similarity hypothesis in the solar wind
Self-preservation
5 - Turbulent energy transfer and proton-electron heating in collisionless plasmas
5.0. Introduction
5.1. The role of pressure-strain interaction in dissipation
5.2. Energy injection and MHD-scale cascade
5.3. MHD-scale energy transfer drives dissipation
5.4. Ion versus electron heating
5.6. Variation of relative heating rates with plasma beta
Chapman-Enskog expansion
Heating by kinetic instabilities
Landau damping
Magnetic pumping
Theory of stochastic heating
Transit-time resonance
6 - Energy dissipation in electron-only reconnection
6.1. Magnetic reconnection
6.2. Structure of the dissipation region in collisionless reconnection
6.3. Electron-only reconnection
6.4. Relation between relative heating rates and the simulation box size
6.5. Relation between pressure-strain interaction and curvature
7 - Scale dependence of energy transfer in collisionless plasmas
7.2. Reconnection
7.3. Turbulence
8 - Future work
8.1. Understanding importance of the transport terms
8.2. Relation between the cross-scale energy transfer and the filtered strain rates
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Boltzmann equation
∂
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α
∂
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+
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⋅
∇
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∇
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=
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