LEADER 05222nam 2200577 a 450 001 9910139026103321 005 20230803021443.0 010 $a3-527-64894-1 010 $a3-527-64892-5 010 $a3-527-64895-X 035 $a(CKB)2550000001111778 035 $a(EBL)1441795 035 $a(OCoLC)861558851 035 $a(MiAaPQ)EBC1441795 035 $a(Au-PeEL)EBL1441795 035 $a(CaPaEBR)ebr10748645 035 $a(CaONFJC)MIL511670 035 $a(EXLCZ)992550000001111778 100 $a20130831d2013 uy 0 101 0 $aeng 135 $aur|n|---||||| 200 10$aMagnetic processes in astrophysics$b[electronic resource] $etheory, simulations, experiments /$fGu?nther Ru?diger, Leonid L. Kitchatinov, and Rainer Hollerbach 205 $a2nd ed. 210 $aWeinheim $cWiley-VCH Verlag GmbH & Co. KGaA$d2013 215 $a1 online resource (358 p.) 300 $aDescription based upon print version of record. 311 $a3-527-41034-1 311 $a1-299-80419-5 320 $aIncludes bibliographical references and index. 327 $aMagnetic 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 327 $a1.6 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 327 $a2.3.4 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 327 $a3.4.2 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 327 $a4.3 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 327 $a5.4 Diffusive Kepler Disks 330 $aIn 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 606 $aMagnetics 606 $aAstrophysics 615 0$aMagnetics. 615 0$aAstrophysics. 676 $a523.0188 700 $aRu?diger$b G$g(Gu?nther)$052846 701 $aKitchatinov$b Leonid L$0924725 701 $aHollerbach$b Rainer$0924726 801 0$bMiAaPQ 801 1$bMiAaPQ 801 2$bMiAaPQ 906 $aBOOK 912 $a9910139026103321 996 $aMagnetic processes in astrophysics$92075643 997 $aUNINA