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Magnetic Processes in Astrophysics : Theory, Simulations, Experiments.
In this work the authors draw upon their expertise in geophysical and astrophysical MHD to explore the motion of electrically conducting fluids, the so-called dynamo effect, and describe the similarities and differences between different magnetized objects. They also explain why magnetic fields are...
| Clasificación: | Libro Electrónico |
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| Autor principal: | |
| Otros Autores: | , |
| Formato: | Electrónico eBook |
| Idioma: | Inglés |
| Publicado: |
Hoboken :
Wiley,
2013.
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| Edición: | 2nd ed. |
| Temas: | |
| Acceso en línea: | Texto completo |
Tabla de Contenidos:
- Magnetic Processes in Astrophysics; Contents; Preface; 1 Differential Rotation of Stars; 1.1 Solar Observations; 1.1.1 The Rotation Law; 1.1.2 Torsional Oscillations; 1.1.3 Meridional Flow; 1.2 Stellar Observations; 1.2.1 Rotational Evolution; 1.2.2 Differential Rotation; 1.3 The Reynolds Stress; 1.3.1 The Lambda Effect; 1.3.2 Eddy Viscosities; 1.4 The Meridional Flow; 1.4.1 Origin of the Meridional Flow; 1.4.2 The Differential Temperature; 1.4.3 Advection-Dominated Solar Dynamo; 1.5 The Sun; 1.5.1 Sun without Lambda Effect; 1.5.2 Sun without Baroclinic Flow; 1.5.3 Global Simulations.
- 1.6 Individual Stars1.6.1 Two Most Stars; 1.6.2 Young Stars; 1.7 Dwarfs & Giants; 1.7.1 M Dwarfs; 1.7.2 F Stars; 1.7.3 Giants; 1.8 Differential Rotation along the Main Sequence; 2 Radiation Zones: Magnetic Stability and Rotation; 2.1 The Watson Problem; 2.1.1 The Stability Equations; 2.1.2 2D Approximation; 2.1.3 Stability Maps; 2.2 The Magnetic Tachocline; 2.2.1 A Planar Model; 2.2.2 Magnetic Field Confinement by Meridional Flow; 2.2.3 Tachocline Model in Spherical Geometry; 2.3 Stability of Toroidal Fields; 2.3.1 Equations; 2.3.2 Nonexistence of 2D Magnetic Instabilities; 2.3.3 No Diffusion.
- 2.3.4 Growth Rates, Drift Rates and Radial Mixing2.4 Stability of Thin Toroidal Field Belts; 2.4.1 Rigid Rotation; 2.4.2 Differential Rotation; 2.4.3 High Fourier Modes; 2.5 Helicity and Dynamo Action; 2.5.1 Helicity and Alpha Effect; 2.5.2 Dynamo Action; 2.6 Ap Star Magnetism; 2.7 The Shear-Hall Instability (SHI); 3 Quasi-linear Theory of Driven Turbulence; 3.1 The Turbulence Pressure; 3.2 The -Tensor; 3.2.1 Rotating Turbulence; 3.2.2 Nonrotating Turbulence but Helical Background Fields; 3.3 Kinetic Helicity and DIV-CURL Correlation; 3.4 Cross-Helicity; 3.4.1 Theory.
- 3.4.2 Simulations and Observations3.5 Shear Flow Electrodynamics; 3.5.1 Hydrodynamic Stability of Shear Flow; 3.5.2 The Magnetic-Diffusivity Tensor; 3.5.3 Dynamos without Stratification; 3.6 The Alpha Effect; 3.6.1 Helical-driven Turbulence; 3.6.2 Shear Flow; 3.6.3 Shear-Dynamos with Turbulence-Stratification; 3.6.4 Alpha Effect by Density Stratification; 3.7 The Current Helicity; 4 The Galactic Dynamo; 4.1 Magnetic Fields of Galaxies; 4.2 Interstellar Turbulence; 4.2.1 Hydrostatic Equilibrium and Interstellar Turbulence; 4.2.2 Alpha Effect by Supernova Explosions; 4.2.3 The Advection Problem.
- 4.3 Dynamo Models4.3.1 Linear Models; 4.3.2 Nonlinear Dynamo Models; 4.4 Magnetic Instabilities; 4.4.1 The Seed Field Problem; 4.4.2 Magnetorotational Instability; 4.4.3 Tayler Instability; 5 The Magnetorotational Instability (MRI); 5.1 Taylor-Couette Flows; 5.2 The Stratorotational Instability (SRI); 5.2.1 The Angular Momentum Transport; 5.2.2 Electromotive Force by Magnetized SRI; 5.3 The Standard Magnetorotational Instability (SMRI); 5.3.1 The Equations; 5.3.2 Nonaxisymmetric Modes; 5.3.3 Wave Numbers; 5.3.4 Nonlinear Simulations; 5.3.5 The Angular Momentum Transport.