Stellar Magnetism

Name: Stellar Magnetism | Second Edition
Brand: OUP Oxford
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Second Edition

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Erschienen am 16. Februar 2012

740 Seiten

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Inhalt

Cover
Contents
Figure acknowledgements
Abbreviations in Reference Lists
1 Introduction
1.1 Historical survey
1.2 Stellar magnetic fields
Bibliography
2 Theoretical basis
2.1 Maxwell's equations and the magnetohydrodynamic approximation
2.2 Properties of cosmical plasmas
2.3 Macroscopic equations for a fully ionized gas: the two-fiuid model
2.3.1 Equations to the flow of the whole gas
2.3.2 The generalized Ohm's law
2.4 The energy equation of a fully ionized gas
2.5 Kinematic coupling
2.6 Dynamical coupling
2.7 The three-fluid model
2.8 'Anomalous' resistivity
Bibliography
3 Applications
3.1 Magnetosonic waves
3.2 Magnetohydrodynamic shocks
3.3 Self-gravitating systems: the virial theorems
3.4 Magnetostatic equilibrium: force-free fields
3.5 Magnetic helicity
3.6 Stability
3.6.1 The MHD energy principle
3.6.2 Illustrative examples
3.6.3 The pinched cylindrical discharge
3.6.4 The Kelvin-Helmholtz instability
3.6.5 Stability of rotating systems
3.7 Effects of dissipation: reconnection
3.7.1 Reconnection in a medium at rest
3.7.2 The Sweet-Parker model
3.7.3 Fast reconnection
3.7.4 Hall reconnection
3.8 Macroscopic dissipation
Appendix: Poloidal and toroidal fields
Bibliography
4 Magnetism and convection
4.1 Introduction
4.2 The angular velocity distribution in a convective zone
4.2.1 The Reynolds stresses
4.2.2 Departure from adiabaticity
4.3 The effect of convective motions on an imposed magnetic field
4.4 A strong imposed field and the onset of convection
4.4.1 Imposed field vertical
4.4.2 Imposed field horizontal
4.5 Non-linear theory: recent developments
4.5.1 The non-magnetic problem
4.5.2 Magnetoconvection
4.6 Sunspots, pores, and isolated flux tubes
4.7 Magnetic buoyancy
4.7.1 Flux tubes
4.7.2 Instability in magnetically supported domains
4.7.3 Non-linear developments
4.8 Solar activity
4.8.1 Flux tube dynamics
4.8.2 Chromospheric and coronal MHD
Bibliography
5 Magnetic fields in stellar interiors
5.1 General considerations
5.2 Magnetic fields and stellar rotation
5.2.1 Axisymmetric states
5.2.2 'Quasi-steady', non-axisymmetric states
5.3 Stability
5.4 Laminar meridian flow in radiative domains
5.5 The interaction between rotation, magnetism, and circulation
5.5.1 Steady-state integrals
5.5.2 Equatorial acceleration
5.5.3 The approach to a quasi-steady state
5.6 Ohmic decay of primeval magnetic fields
5.6.1 Decay of a purely poloidal field
5.6.2 Decay of a mixed poloidal-toroidal field
5.7 The Biermann 'battery' process
5.7.1 Coupling with a poloidal field
5.7.2 The effect of chemical inhomogeneities
5.8 An introduction to the stellar dynamo problem
5.8.1 Cowling's anti-dynamo theorem
5.8.2 Mass motions and the rate of decay
Bibliography
6 Dynamo processes in stars
6.1 Introduction
6.2 Laminar kinematic dynamos
6.3 The Parker model
6.4 Turbulent dynamos
6.4.1 Mean-field electrodynamics: the classical treatment
6.4.2 Isotropic turbulence
6.4.3 Kinematics and dynamics in the low Reynolds number domain
6.5 Kinematic models of the turbulent dynamo
6.5.1 General discussion
6.5.2 The aO dynamo
6.5.3 A model with separate shear and a-effect zones
6.6 Non-linear dynamical feedback
6.6.1 Buoyancy-limited growth
6.6.2 Magnetic back-reaction: modulated cycles
6.7 Fundamental problems
6.7.1 The a-effect and helicity
6.7.2 The dynamical back-reaction
6.7.3 Analytical treatment
6.8 The role of magnetic helicity in the dynamo problem
6.8.1 Magnetic helicity evolution
6.8.2 Dynamical a-quenching in closed or periodic domians
6.8.3 Mean-field models with magnetic helicity flux
6.9 Numerical simulations
6.9.1 a- and ?-quenching
6.9.2 Further numerical work: a return to first principles
6.10 Dynamo action guided by a strong pre-existing field
6.10.1 A dynamo driven by the instability of strong flux tubes
6.10.2 A two-dimensional flux tube model
6.11 Conclusions
Bibliography
7 Stellar winds: magnetic braking
7.1 Introduction
7.2 The braking of axisymmetric systems
7.3 The wind theory
7.4 The structure of the poloidal field
7.4.1 General discussion
7.4.2 A numerical attack
7.4.3 Asymptotic behaviour
7.5 A simple field model
7.6 The rate of braking
7.7 A digression on the micro-physics
7.8 Magnetic braking of the oblique rotator
7.8.1 The generalized wind theory
7.8.2 The gross dynamics of the star
7.8.3 The effect of the thermo-centrifugal wind
7.9 Winds driven by Alfvén waves
7.10 The solar wind revisited
7.11 Radiation-driven winds from hot early-type stars
Appendix A: Alfvén waves in a multi-component plasma
Appendix B: The axisymmetric magnetic rotator: the energetics
Bibliography
8 Late-type stars
8.1 Introduction
8.2 The 'solar-stellar connection'
8.2.1 The rapidly rotating dwarf star AB Doradus
8.3 The rotational history of late-type main-sequence stars
8.4 The Sun: new observational material
8.4.1 Solar activity: the solar cycle
8.4.2 The internal solar rotation
8.5 Phenomenological studies of the solar dynamo
8.6 The solar dynamo revisited
8.6.1 Historical résumé
8.6.2 Current ideas on the solar dynamo
8.7 Further recent computations
8.7.1 The rotation of the convective envelope
8.7.2 Dynamo action
8.8 The tachocline
8.8.1 Non-magnetic theory
8.8.2 Subsequent developments: gyroscopic pumping and magnetohydrodynamic theory
8.8.3 A slow tachocline dynamo
8.8.4 Application to tachocline dynamics
8.8.5 The 'Li problem'
8.8.6 Résumé
8.8.7 Subsequent developments
8.9 The solar-stellar connection revisited
8.9.1 Sub-solar-mass stars
8.9.2 Young solar-mass stars
8.10 Return to the standard dynamo equations
8.10.1 Modulation of cyclic activity
8.10.2 Rapidly rotating late-type stars
8.10.3 Evolved stars
8.10.4 Non-axisymmetric field generation
Bibliography
9 The early-type magnetic stars
9.1 The basic observational data: historical summary
9.1.1 Field-structure modelling
9.1.2 Correlations
9.1.3 Evolution
9.1.4 Problems
9.2 Stability of large-scale stellar magnetic fields
9.3 The dynamics of the oblique rotator: the Eulerian nutation and the consequent internal motions
9.3.1 The construction of a unique ?-field
9.3.2 Consequences of the ?-motions
9.3.3 Dissipation of the ?-motions
9.4 Non-uniform rotation and the oblique rotator model
9.5 Models of rotating magnetic stars
9.5.1 Axisymmetric radiative zones
9.5.2 Models with thermally-driven circulation
9.5.3 Generalizations
9.6 Magnetic torques acting on the oblique rotator: spin-down, spin-up, and changes in obliquity
9.6.1 Braking processes in the pre-main-sequence and main-sequence epochs
9.6.2 Changes in obliquity
9.7 The origin of the field
9.7.1 Recapitulation
9.8 Abundance anomalies
9.9 The roAp phenomenon
Appendix A: Stellar atmospheres
Appendix B: Evolution of a dynamically stable magnetic field: an analytical treatment
Bibliography
General references
10 Pre-main-sequence stars
10.1 The later stages of star formation
10.2 Magnetic accretion discs
10.2.1 The magnetosphere
10.2.2 Canonical disc theory: angular momentum transport
10.2.3 An illustrative model
10.2.4 The estimated net torque
10.3 Pre-main-sequence rotational evolution
10.4 Later developments
10.4.1 X-ray observations
10.4.2 Accretion disc theory: later developments
10.4.3 Models with reduced magnetic coupling between star and disc
10.4.4 Numerical simulations
10.4.5 Disc locking
10.5 Instability in a magnetic rotating disc
10.5.1 The magneto-rotational instability
10.5.2 A more formal treatment
10.5.3 Angular momentum transport in a thin radiative disc
10.6 Disc dynamos
10.6.1 Applications of the 'standard dynamo equations'
10.6.2 Dynamo action driven by the magneto-rotational instability
10.6.3 Comments and queries
10.7 Centrifugal winds from discs
10.7.1 Cold, centrifugally-driven winds
10.7.2 The flow near the disc surface
10.8 Collimation
10.8.1 Toroidal field collimation
10.8.2 Detailed models
10.8.3 Collimation by the poloidal field
10.9 Conclusion
Appendix A: The model of Section 10.2: canonical disc theory
Appendix B: Other instabilities in discs
Bibliography
11 Magnryism and star formation I
11.1 Introduction
11.2 Magneto-thermo-gravitational equilibrium
11.2.1 A spherical cloud model
11.2.2 A spheroidal model
11.2.3 Résumé
11.3 Applications
11.3.1 The accumulation length
11.3.2 The B-? relations in a cool cloud
11.3.3 Strongly turbulent clouds
11.4 Gravitational collapse under flux-freezing: possible fragmentation
11.5 The angular momentum problem
11.6 Magnetic braking by Alfvén waves
11.6.1 An axisymmetric cylindrical model
11.6.2 Braking by a radially distorted field
11.6.3 Magnetic braking and gravitational contraction
11.6.4 A perpendicular magnetic rotator
11.6.5 Fragmentation of a rotating magnetic cloud
11.7 Flux leakage
11.7.1 Ambipolar diffusion
11.7.2 Quasi-steady contraction of an oblate spheroidal model
Appendix A: The model of Figure 11.2
Appendix B: Magnetic braking by Alfvén waves: detailed treatment
12 Magnetism and star formation II
12.1 Résumé
12.2 Magneto-gravitational equilibrium: exact disc-like models
12.2.1 Finite disc models
12.2.2 Infinite disc models
12.2.3 Collapsed core models
12.2.4 Disc models with partial turbulent support
12.2.5 Magneto-gravitational equilibrium: summary
12.3 Magneto-turbulent cloud models
12.4 Evolution through flux diffusion
12.5 Gravitational collapse
12.6 Field line detachment
12.7 Flux leakage
12.8 Magnetic 'levitation'
12.9 Alfvénic turbulence
12.9.1 Non-dissipative theory
12.9.2 The effect of dissipation
12.10 Turbulent ambipolar diffusion
12.11 The future
12.11.1 Magneto-turbulence and star formation
12.12 Summary
Appendix A: Exact disc-like models
Appendix B: Magnetized singular isothermal toroids
Appendix C: Isopedic disc models
Appendix D: Turbulent ambipolar diffusion
Bibliography (Chapters 11 and 12)
Index
A
B
C
D
E
F
G
H
I
M
O
P
R
S
T
Z

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