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...

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Detalles Bibliográficos
Clasificación:Libro Electrónico
Autor principal: Rüdiger, G. (Günther)
Otros Autores: Hollerbach, Rainer, Kitchatinov, Leonid L.
Formato: Electrónico eBook
Idioma:Inglés
Publicado: Hoboken : Wiley, 2013.
Edición:2nd ed.
Temas:
Nuclear astrophysics.
Astrophysique nucléaire.
Nuclear astrophysics
Acceso en línea:Texto completo

MARC

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245 1 0 |a Magnetic Processes in Astrophysics :  |b Theory, Simulations, Experiments. 
250 |a 2nd ed. 
260 |a Hoboken :  |b Wiley,  |c 2013. 
300 |a 1 online resource (358 pages) 
336 |a text  |b txt  |2 rdacontent 
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505 0 |a 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. 
505 8 |a 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. 
505 8 |a 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. 
505 8 |a 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. 
505 8 |a 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. 
500 |a 5.4 Diffusive Kepler Disks. 
520 |a 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 crucial to the formation of the stars, and discuss promising experiments currently being designed to investigate some of the relevant physics in the laboratory. This interdisciplinary approach will appeal to a wide audience in physics, astrophysics and geophysics. This second edition covers such. 
588 0 |a Print version record. 
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650 0 |a Nuclear astrophysics. 
650 6 |a Astrophysique nucléaire. 
650 7 |a Nuclear astrophysics  |2 fast 
700 1 |a Hollerbach, Rainer. 
700 1 |a Kitchatinov, Leonid L. 
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776 0 8 |i Print version:  |a Rüdiger, Günther.  |t Magnetic Processes in Astrophysics : Theory, Simulations, Experiments.  |d Hoboken : Wiley, ©2013  |z 9783527410347 
856 4 0 |u https://ebookcentral.uam.elogim.com/lib/uam-ebooks/detail.action?docID=1441795  |z Texto completo 
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