Muutke küpsiste eelistusi

E-raamat: Stellar Magnetism: Second Edition 2nd Revised edition [Oxford Scholarship Online e-raamatud]

(Emeritus Professor of Astronomy, University of Sussex)
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Stellar Magnetism: Second Edition 2nd Revised editionSuurem pilt
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Ongoing studies in mathematical depth, and inferences from `helioseismological' observations of the internal solar rotation have shown up the limitations in our knowledge of the solar interior and of our understanding of the solar dynamo, manifested in particular by the sunspot cycle, the Maunder minimum, and solar flares. This second edition retains the identical overall structure as the first edition, but is designed so as to be self-contained with the early chapters presenting the basic physics and mathematics underlying cosmical magnetohydrodynamics, followed by studies of the specific applications appropriate for a book devoted to a central area in astrophysics.

New to this edition:
Chapter 6 gives an account of the present state of dynamo theory in general, and Chapter 8 the applications to the Sun and to other `Late-Type' stars with differing rotation rates -- the `Solar-Stellar Connection'. The minority of the more massive `Early-Type' stars that are observably magnetic are well described by the`oblique rotator' model, with a quasi-steady, `fossil' magnetic structure `frozen' into the highly conducting, non-turbulent envelope. Chapter 9 deals with the considerable progress on the associated theoretical problems.
Chapter 7 contains new material, relevant to both Late- and Early-Type Main Sequence stars, to the evolved Red Giants, and also to contracting pre-Main Sequence stars (Chapter 10}, which show the highest degree of magnetic activity (the magneto-rotational instability, and the magneto-centrifugal winds emitted by the surrounding `accretion disk'). In the earlier phases of star formation in molecular clouds (Chapters 11-12), `magneto-turbulence' is emerging as the appropriate scenario for the prediction of the mass spectrum of proto-stars, and the associated formation of planetary satellites. Chapter 14 describes developments in the study of the magnetosphere of a `pulsar' -- a magnetized neutron star -- consisting of spontaneously generated electron-positron pairs.
Figure acknowledgements
xvi
Abbreviations in Reference Lists xx
1 Introduction
1(12)
1.1 Historical survey
1(5)
1.2 Stellar magnetic fields
6(7)
Bibliography
11(2)
2 Theoretical basis
13(32)
2.1 Maxwell's equations and the magnetohydrodynamic approximation
13(3)
2.2 Properties of cosmical plasmas
16(3)
2.3 Macroscopic equations for a fully ionized gas: the two-fluid model
19(8)
2.3.1 Equations to the flow of the whole gas
20(3)
2.3.2 The generalized Ohm's law
23(4)
2.4 The energy equation of a fully ionized gas
27(2)
2.5 Kinematic coupling
29(4)
2.6 Dynamical coupling
33(4)
2.7 The three-fluid model
37(3)
2.8 `Anomalous' resistivity
40(5)
Bibliography
43(2)
3 Applications
45(59)
3.1 Magnetosonic waves
45(2)
3.2 Magnetohydrodynamic shocks
47(5)
3.3 Self-gravitating systems: the virial theorems
52(6)
3.4 Magnetostatic equilibrium: force-free fields
58(7)
3.5 Magnetic helicity
65(4)
3.6 Stability
69(15)
3.6.1 The MHD energy principle
69(2)
3.6.2 Illustrative examples
71(3)
3.6.3 The pinched cylindrical discharge
74(5)
3.6.4 The Kelvin--Helmholtz instability
79(3)
3.6.5 Stability of rotating systems
82(2)
3.7 Effects of dissipation: reconnection
84(13)
3.7.1 Reconnection in a medium at rest
85(3)
3.7.2 The Sweet--Parker model
88(3)
3.7.3 Fast reconnection
91(4)
3.7.4 Hall reconnection
95(2)
3.8 Macroscopic dissipation
97(7)
Appendix: Poloidal and toroidal fields
99(1)
Bibliography
100(4)
4 Magnetism and convection
104(56)
4.1 Introduction
104(4)
4.2 The angular velocity distribution in a convective zone
108(7)
4.2.1 The Reynolds stresses
108(3)
4.2.2 Departure from adiabaticity
111(4)
4.3 The effect of convective motions on an imposed magnetic field
115(5)
4.4 A strong imposed field and the onset of convection
120(4)
4.4.1 Imposed field vertical
120(3)
4.4.2 Imposed field horizontal
123(1)
4.5 Non-linear theory: recent developments
124(10)
4.5.1 The non-magnetic problem
125(4)
4.5.2 Magnetoconvection
129(5)
4.6 Sunspots, pores, and isolated flux tubes
134(3)
4.7 Magnetic buoyancy
137(4)
4.7.1 Flux tubes
137(2)
4.7.2 Instability in magnetically supported domains
139(1)
4.7.3 Non-linear developments
140(1)
4.8 Solar activity
141(19)
4.8.1 Flux tube dynamics
142(6)
4.8.2 Chromospheric and coronal MHD
148(5)
Bibliography
153(7)
5 Magnetic fields in stellar interiors
160(41)
5.1 General considerations
160(2)
5.2 Magnetic fields and stellar rotation
162(5)
5.2.1 Axisymmetric states
162(4)
5.2.2 `Quasi-steady', non-axisymmetric states
166(1)
5.3 Stability
167(4)
5.4 Laminar meridian flow in radiative domains
171(5)
5.5 The interaction between rotation, magnetism, and circulation
176(7)
5.5.1 Steady-state integrals
176(3)
5.5.2 Equatorial acceleration
179(1)
5.5.3 The approach to a quasi-steady state
180(3)
5.6 Ohmic decay of primeval magnetic fields
183(5)
5.6.1 Decay of a purely poloidal field
183(2)
5.6.2 Decay of a mixed poloidal--toroidal field
185(3)
5.7 The Biermann `battery' process
188(5)
5.7.1 Coupling with a poloidal field
189(2)
5.7.2 The effect of chemical inhomogeneities
191(2)
5.8 An introduction to the stellar dynamo problem
193(8)
5.8.1 Cowling's anti-dynamo theorem
193(3)
5.8.2 Mass motions and the rate of decay
196(2)
Bibliography
198(3)
6 Dynamo processes in stars
201(62)
6.1 Introduction
201(2)
6.2 Laminar kinematic dynamos
203(4)
6.3 The Parker model
207(3)
6.4 Turbulent dynamos
210(12)
6.4.1 Mean-field electrodynamics: the classical treatment
210(7)
6.4.2 Isotropic turbulence
217(2)
6.4.3 Kinematics and dynamics in the low Reynolds number domain
219(3)
6.5 Kinematic models of the turbulent dynamo
222(8)
6.5.1 General discussion
222(2)
6.5.2 The αΩ dynamo
224(1)
6.5.3 A model with separate shear and α-effect zones
225(5)
6.6 Non-linear dynamical feedback
230(6)
6.6.1 Buoyancy-limited growth
230(2)
6.6.2 Magnetic back-reaction: modulated cycles
232(4)
6.7 Fundamental problems
236(5)
6.7.1 The α-effect and helicity
236(2)
6.7.2 The dynamical back-reaction
238(1)
6.7.3 Analytical treatment
239(2)
6.8 The role of magnetic helicity in the dynamo problem
241(5)
6.8.1 Magnetic helicity evolution
241(2)
6.8.2 Dynamical α-quenching in closed or periodic domains
243(2)
6.8.3 Mean-field models with magnetic helicity flux
245(1)
6.9 Numerical simulations
246(4)
6.9.1 α- and η-quenching
246(2)
6.9.2 Further numerical work: a return to first principles
248(2)
6.10 Dynamo action guided by a strong pre-existing field
250(6)
6.10.1 A dynamo driven by the instability of strong flux tubes
251(3)
6.10.2 A two-dimensional flux tube model
254(2)
6.11 Conclusions
256(7)
Bibliography
257(6)
7 Stellar winds: magnetic braking
263(50)
7.1 Introduction
263(2)
7.2 The braking of axisymmetric systems
265(2)
7.3 The wind theory
267(3)
7.4 The structure of the poloidal field
270(10)
7.4.1 General discussion
270(3)
7.4.2 A numerical attack
273(3)
7.4.3 Asymptotic behaviour
276(4)
7.5 A simple field model
280(4)
7.6 The rate of braking
284(2)
7.7 A digression on the micro-physics
286(3)
7.8 Magnetic braking of the oblique rotator
289(6)
7.8.1 The generalized wind theory
289(3)
7.8.2 The gross dynamics of the star
292(1)
7.8.3 The effect of the thermo-centrifugal wind
293(2)
7.9 Winds driven by Alfven waves
295(6)
7.10 The solar wind revisited
301(3)
7.11 Radiation-driven winds from hot early-type stars
304(9)
Appendix A Alfven waves in a multi-component plasma
307(1)
Appendix B The axisymmetric magnetic rotator: the energetics
308(2)
Bibliography
310(3)
8 Late-type stars
313(94)
8.1 Introduction
313(2)
8.2 The `solar-stellar connection'
315(7)
8.2.1 The rapidly rotating dwarf star AB Doradus
319(3)
8.3 The rotational history of late-type main-sequence stars
322(8)
8.4 The Sun: new observational material
330(6)
8.4.1 Solar activity: the solar cycle
330(2)
8.4.2 The internal solar rotation
332(4)
8.5 Phenomenological studies of the solar dynamo
336(3)
8.6 The solar dynamo revisited
339(6)
8.6.1 Historical resume
339(4)
8.6.2 Current ideas on the solar dynamo
343(2)
8.7 Further recent computations
345(10)
8.7.1 The rotation of the convective envelope
345(6)
8.7.2 Dynamo action
351(4)
8.8 The tachocline
355(20)
8.8.1 Non-magnetic theory
355(3)
8.8.2 Subsequent developments: gyroscopic pumping and magnetohydrodynamic theory
358(5)
8.8.3 A slow tachocline dynamo
363(5)
8.8.4 Application to tachocline dynamics
368(2)
8.8.5 The `Li problem'
370(1)
8.8.6 Resume
371(2)
8.8.7 Subsequent developments
373(2)
8.9 The solar--stellar connection revisited
375(4)
8.9.1 Sub-solar-mass stars
375(2)
8.9.2 Young solar-mass stars
377(2)
8.10 Return to the standard dynamo equations
379(28)
8.10.1 Modulation of cyclic activity
380(7)
8.10.2 Rapidly rotating late-type stars
387(5)
8.10.3 Evolved stars
392(2)
8.10.4 Non-axisymmetric field generation
394(2)
Bibliography
396(11)
9 The early-type magnetic stars
407(89)
9.1 The basic observational data: historical summary
407(8)
9.1.1 Field-structure modelling
409(3)
9.1.2 Correlations
412(1)
9.1.3 Evolution
413(1)
9.1.4 Problems
414(1)
9.2 Stability of large-scale stellar magnetic fields
415(2)
9.3 The dynamics of the oblique rotator: the Eulerian nutation and the consequent internal motions
417(11)
9.3.1 The construction of a unique ξ-field
421(3)
9.3.2 Consequences of the ξ-motions
424(1)
9.3.3 Dissipation of the ξ-motions
425(3)
9.4 Non-uniform rotation and the oblique rotator model
428(3)
9.5 Models of rotating magnetic stars
431(7)
9.5.1 Axisymmetric radiative zones
432(1)
9.5.2 Models with thermally-driven circulation
433(2)
9.5.3 Generalizations
435(3)
9.6 Magnetic torques acting on the oblique rotator: spin-down, spin-up, and changes in obliquity
438(11)
9.6.1 Braking processes in the pre-main-sequence and main-sequence epochs
438(4)
9.6.2 Changes in obliquity
442(7)
9.7 The origin of the field
449(7)
9.7.1 Recapitulation
453(3)
9.8 Abundance anomalies
456(4)
9.9 The roAp phenomenon
460(36)
Appendix A Stellar atmospheres
463(1)
A1 The atmospheres of non-magnetic stars
463(3)
A2 Magnetic star atmospheres
466(6)
Appendix B Evolution of a dynamically stable magnetic field: an analytical treatment
472(17)
Bibliography
489(6)
General references
495(1)
10 Pre-main-sequence stars
496(80)
10.1 The later stages of star formation
496(5)
10.2 Magnetic accretion discs
501(9)
10.2.1 The magnetosphere
502(2)
10.2.2 Canonical disc theory: angular momentum transport
504(2)
10.2.3 An illustrative model
506(2)
10.2.4 The estimated net torque
508(2)
10.3 Pre-main-sequence rotational evolution
510(6)
10.4 Later developments
516(6)
10.4.1 X-ray observations
516(1)
10.4.2 Accretion disc theory: later developments
517(1)
10.4.3 Models with reduced magnetic coupling between star and disc
518(2)
10.4.4 Numerical simulations
520(1)
10.4.5 Disc locking
521(1)
10.5 Instability in a magnetic rotating disc
522(10)
10.5.1 The magneto-rotational instability
523(3)
10.5.2 A more formal treatment
526(4)
10.5.3 Angular momentum transport in a thin radiative disc
530(2)
10.6 Disc dynamos
532(6)
10.6.1 Applications of the `standard dynamo equations'
532(4)
10.6.2 Dynamo action driven by the magneto-rotational instability
536(2)
10.6.3 Comments and queries
538(1)
10.7 Centrifugal winds from discs
538(7)
10.7.1 Cold, centrifugally-driven winds
539(3)
10.7.2 The flow near the disc surface
542(3)
10.8 Collimation
545(12)
10.8.1 Toroidal field collimation
545(3)
10.8.2 Detailed models
548(6)
10.8.3 Collimation by the poloidal field
554(3)
10.9 Conclusion
557(19)
Appendix A The model of Section 10.2: canonical disc theory
557(7)
Appendix B Other instabilities in discs
564(5)
Bibliography
569(7)
11 Magnetism and star formation I
576(60)
11.1 Introduction
576(4)
11.2 Magneto-thermo-gravitational equilibrium
580(9)
11.2.1 A spherical cloud model
580(3)
11.2.2 A spheroidal model
583(6)
11.2.3 Resume
589(1)
11.3 Applications
589(6)
11.3.1 The accumulation length
58(533)
11.3.2 The B--p relations in a cool cloud
591(3)
11.3.3 Strongly turbulent clouds
594(1)
11.4 Gravitational collapse under flux-freezing: possible fragmentation
595(6)
11.5 The angular momentum problem
601(4)
11.6 Magnetic braking by Alfven waves
605(9)
11.6.1 An axisymmetric cylindrical model
605(3)
11.6.2 Braking by a radially distorted field
608(2)
11.6.3 Magnetic braking and gravitational contraction
610(2)
11.6.4 A perpendicular magnetic rotator
612(1)
11.6.5 Fragmentation of a rotating magnetic cloud
613(1)
11.7 Flux leakage
614(22)
11.7.1 Ambipolar diffusion
614(5)
11.7.2 Quasi-steady contraction of an oblate spheroidal model
619(4)
Appendix A The model of Figure 11.2
623(4)
Appendix B Magnetic braking by Alfven waves: detailed treatment
627(9)
12 Magnetism and star formation II
636(74)
12.1 Resume
636(4)
12.2 Magneto-gravitational equilibrium: exact disc-like models
640(14)
12.2.1 Finite disc models
640(5)
12.2.2 Infinite disc models
645(3)
12.2.3 Collapsed core models
648(2)
12.2.4 Disc models with partial turbulent support
650(3)
12.2.5 Magneto-gravitational equilibrium: summary
653(1)
12.3 Magneto-turbulent cloud models
654(3)
12.4 Evolution through flux diffusion
657(3)
12.5 Gravitational collapse
660(1)
12.6 Field line detachment
661(2)
12.7 Flux leakage
663(1)
12.8 Magnetic `levitation'?
664(7)
12.9 Alfvenic turbulence
671(8)
12.9.1 Non-dissipative theory
671(5)
12.9.2 The effect of dissipation
676(3)
12.10 Turbulent ambipolar diffusion
679(1)
12.11 The future
680(4)
12.11.1 Magneto-turbulence and star formation
680(4)
12.12 Summary
684(26)
Appendix A Exact disc-like models
687(5)
Appendix B Magnetized singular isothermal toroids
692(4)
Appendix C Isopedic disc models
696(3)
Appendix D Turbulent ambipolar diffusion
699(5)
Bibliography (Chapters 11 and 12)
704(6)
Index 710
Leon Mestel is Emeritus Professor of Astronomy at the University of Sussex. Mestel has also taught at the University of Cambridge, Princeton University, the Weizmann Institute in Rehovoth, Israel, the University of Manchester, and the Racah Institue at the Hebrew University in Jerusalem. He has established himself as one of the leaders in his field.
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