Cover
Half-title
Title
Copyright
Contents
Preface
1 A selective overview
1.1 Introduction
1.2 On taking mixing-length theory seriously
1.3 The solar spoon
1.4 Deep roots of solar cycles
1.5 Helioseismology: oscillations as a diagnostic of the solar interior
1.6 Inverting helioseismic data
1.7 On the detection of subphotospheric convective velocities and temperature fluctuations
1.8 Prospects for asteroseismic inference
References
I Stellar convection and oscillations
2 On the diversity of stellar pulsations
2.1 Introduction
2.2 Types of stellar pulsation
2.2.1 Giant-type pulsators
2.3 Dwarf-type pulsators
2.4 Inference from linear theory
2.5 Saturation of the linear instability
2.6 Amplitude limitation by resonances
2.6.1 The 2:1 resonance
2.6.2 Parametric resonance and dwarf and giant dichotomy
2.6.3 Higher-order parametric resonance and the Blazkho effect
2.7 Final remarks
References
3 Acoustic radiation and mode excitation by turbulent convection
3.1 Introduction
3.2 Linear damping rates, Gamma
3.3 Stochastic excitation
3.4 Acoustic radiation in the equilibrium model
References
4 Understanding roAp stars
4.1 Introduction
4.2 Magnetic field versus convection
4.3 Mode excitation and eigenfrequencies
4.3.1 Excitation
4.3.2 Effect on the power spectrum
4.4 Theoretical instability strip
4.5 roAp stars versus noAp stars
4.5.1 noAp stars: are they stable against high frequency pulsations?
4.5.2 noAp stars: why would we fail to observe their oscillations?
4.6 Conclusions
References
5 Waves in the magnetised solar atmosphere
5.1 Introduction
5.2 Description of the models
5.3 Network and internetwork oscillations
5.3.1 Internetwork oscillations
5.3.2 Waves in a network element
5.4 Waves in a weak flux-tube
5.5 Conclusions
References
II Stellar rotation and magnetic fields
6 Stellar rotation: a historical survey
Prologue
6.1 Radiative zones: the Eddington-Vogt-Sweet theory
6.2 Comparison with geophysical theory
6.3 Steady circulation and the mixing problem
6.4 The angular momentum distribution in a radiative zone
6.4.1 Magnetic radiative zones
6.4.2 Non-magnetic radiative zones
6.5 Rotating convective zones
6.6 The solar tachocline
References
7 The oscillations of rapidly rotating stars
7.1 A short introduction to rapidly rotating stars
7.2 Perturbative versus non-perturbative methods
7.3 The part played by the Coriolis acceleration
7.4 The part played by centrifugal acceleration
7.5 Conclusions
References
8 Solar tachocline dynamics: eddy viscosity, anti-friction, or something in between?
8.1 Introduction
8.2 Long-range and short-range momentum transport
8.3 Potential vorticity
8.4 A glimpse of the Earthβs stratosphere
8.5 Turbulence requires waves
8.6 Concluding remarks
References
9 Dynamics of the solar tachocline
9.1 Introduction
9.2 One half of the problem: shear propagation into a rotating stratified fluid
9.2.1 Slow rotating caseβ¦
9.2.3 Solar rotation rate
9.2.4 Discussion
9.3 The other half of the problem: nonlinear interaction between a large-scale field and flows in a rotating sphere
9.4 Conclusion
References
10 Dynamo processes: the interaction of turbulence and magnetic fields
10.1 Scales for solar magnetic fields
10.2 Field structure in kinematic dynamos at large R
10.3 Dynamical equilibration of small-scale dynamos
10.4 Growth and equilibration of mean fields
10.5 Conclusion
References
11 Dynamos in planets
11.1 Introduction
11.2 Planetary magnetic fields
11.3 Convective driving and thermal history
11.4 Physical nature of convective dynamo solutions
11.5 Dynamical regimes in planetary cores
11.6 Conclusions
References
III Physics and structure of stellar interiors
12 Solar constraints on the equation of state
12.1 Introduction
12.2 Equation of state issues
12.2.1 Coulomb correction
12.2.2 Relativistic electrons
12.2.3 Effect of excited states in hydrogen and helium
12.2.4 Heavy elements
12.3 Resolution power of helioseismology
12.4 Conclusions
References
13 He transport and the solar neutrino problem
13.1 Introduction
13.2 Neutrinos and the neutrino problem
13.3 Cumming and Haxtonβs model
13.4 Modelling the flow
13.5 The equations
13.6 Results
13.7 Conclusions
References
14 Mixing in stellar radiation zones
14.1 The observational evidence
14.2 Possible causes of mixing
14.2.1 Convective overshoot and penetration
14.2.2 Meridional circulation
14.2.3 Turbulence caused by differential rotation
14.2.3.1 Turbulence produced by the vertical shear
14.2.3.2 Turbulence produced by the horizontal shear
14.3 Rotational mixing
14.3.1 Rotational mixing of type I
14.3.2 Rotational mixing of type II
14.3.3 Tachocline mixing
14.4 Open questions
14.4.1 Does turbulence caused by a horizontal shear act to reduce that shear?
14.4.2 How does a poloidal field avoid imprinting the differential rotation of the convection zone into the radiation zone?
14.4.3 Can waves extract angular momentum from the solar interior?
References
15 Element settling and rotation-induced mixing in slowly rotating stars
15.1 Introduction
15.2 Element settling in stellar radiative zones
15.2.1 The solar case
15.2.2 The lithium plateau in halo stars
15.3 Rotation-induced mixing in the presence of gravitationally-induced Mu-gradients
15.3.1 Computations of Omega and Mu-currents
15.3.2 Self-regulating process
15.4 Conclusion
References
IV Helio-and asteroseismology
16 Solar structure and the neutrino problem
16.1 Historical review: the solar neutrino problem
16.2 Historical review: helioseismology
16.3 Neutrino oscillation: MSW effect
16.4 SNO and Super-Kamiokande
16.5 Recipe for construction of an evolutionary solar model
16.6 Recipe for construction of a seismic solar model
16.7 Seismic solar model and the neutrino flux estimate
16.8 Future prospects
References
17 Helioseismic data analysis
17.1 Introduction
17.2 Background
17.3 Instruments
17.3.1 GONG
17.3.2 MDI
17.3.3 Other projects
17.4 Normal mode analysis
17.4.1 Time series generation
17.4.2 Peakbagging
17.4.2.1 The MDI algorithm
17.4.2.2 The GONG algorithm
17.4.2.3 Ridge fitting
17.4.3 Analysis problems
17.4.3.1 Bad physics and parameters
17.4.3.2 Instrumental problems
17.4.3.3 Algorithm problems
17.4.3.4 Problems of unknown source
17.4.4 Results
17.5 Supergranulation studies
17.6 Conclusion and future prospects
References
18 Seismology of solar rotation
18.1 Introduction
18.2 Helioseismic measurement of solar internal rotation
18.3 Inversion for internal rotation
18.4 Solar internal rotation observed by helioseismology
18.4.1 Observational data
18.4.2 How to tackle 2-dimensional (2D) inversions
18.4.3 What we have learned
18.5 Rotation in the the solar convection zone
18.6 Line-blending problem
18.7 Summary
References
19 Telechronohelioseismology
19.1 Introduction
19.2 Observational and Theoretical Principles
19.3 Current Inferences
19.3.1 Large-scale flows and solar activity
19.3.2 Developing active regions
19.3.3 Structure and dynamics of sunspots
19.3.4 Far-side imaging
19.4 Conclusion
References
V Large-scale numerical experiments
20 Bridges between helioseismology and models of convection zone dynamics
20.1 Introduction
20.2 Differential rotation: tachocline and near-surface shear
20.3 Solar dynamo: ordered and chaotic emergence of flux
20.4 Tachocline: boundary layer of strong shear
20.5 Contact with 3-D simulations of turbulent convection
20.6 Near-surface shear layer and solar subsurface weather
20.7 Origin of near-surface shear layer
20.8 Reflections
References
21 Numerical simulations of the solar convection zone
21.1 Introduction
21.2 DNS results
21.3 VLES results
21.4 Conclusion
References
22 Modelling solar and stellar magnetoconvection
22.1 Introduction
22.2 Compressible magnetoconvection
22.3 Flux separation
22.4 Small-scale dynamo action
22.5 Conclusion
References
23 Nonlinear magnetoconvection in the presence of a strong oblique field
23.1 Introduction
23.2 Reduced PDE description for Maβ¦
23.2.1 Computational and Theoretical Advantages
23.3 Exact Single-Mode Solutions
23.4 Results
23.5 Conclusion
References
24 Simulations of astrophysical fluids
24.1 Introduction
24.2 Radio relics
24.2.1 Conclusion
24.3 Radio galaxies
References
VI Dynamics
25 A magic electromagnetic field
25.1 The electromagnetic field
25.2 The connection to Kerrβs metric and the electron
25.3 Separability of motion in the field
25.4 Eulogy
References
26 Continuum equations for stellar dynamics
26.1 A kinetic equation
26.2 The collision term
26.3 Fluid equations
26.4 The Jeans instability
26.5 Conclusion
References
27 Formation of planetary systems
27.1 Observations
27.2 Grain condensation and growth
27.3 Planetesimal dynamics
27.4 The final assemblage of terrestrial planets
27.5 Giant planet formation through gas accretion
27.6 Formation of multiple planet systems
References
28 The solar-cycle global warming as inferred from sky brightness variation
28.1 Introduction
28.2 Radiative transfer in the earth atmosphere
28.3 Radiative equilibrium model
28.4 Sky brightness
28.5 Solar-cycle global warming
28.6 Summary
References