
Abstract 
1 
Introduction 

1.1 
Scope of review 

1.2 
What is a “model”? 

1.3 
A brief
historical survey 

1.4 
Sunspots and the butterfly diagram 

1.5 
Organization
of review 
2 
Making a Solar Dynamo Model 

2.1 
Magnetized fluids and
the MHD induction equation 

2.2 
The dynamo problem 

2.3 
Kinematic
models 

2.4 
Axisymmetric formulation 

2.5 
Boundary conditions and
parity 
3 
Mechanisms of Magnetic Field Generation 

3.1 
Poloidal to
toroidal 

3.2 
Toroidal to poloidal 
4 
A Selection of Representative
Models 

4.1 
Model ingredients 

4.2 
meanfield models 

4.3 
Interface
dynamos 

4.4 
Meanfield models including meridional circulation 

4.5 
Models
based on shear instabilities 

4.6 
Models based on buoyant instabilities
of sheared magnetic layers 

4.7 
Models based on flux tube
instabilities 

4.8 
Babcock–Leighton models 

4.9 
Numerical simulations of solar
dynamo action 
5 
Amplitude Fluctuations, Multiperiodicity, and Grand
Minima 

5.1 
The observational evidence: An overview 

5.2 
Fossil fields and the
22yr cycle 

5.3 
Dynamical nonlinearity 

5.4 
Timedelay dynamics 

5.5 
Stochastic
forcing 

5.6 
Intermittency 

5.7 
Solar cycle predictions based on dynamo
models 
6 
Open Questions and Current Trends 

6.1 
What is the primary poloidal
field regeneration mechanism? 

6.2 
What limits the amplitude of the solar
magnetic field? 

6.3 
Flux tubes versus diffuse fields 

6.4 
How constraining is the
sunspot butterfly diagram? 

6.5 
Is meridional circulation crucial? 

6.6 
Is the
mean solar magnetic field really axisymmetric? 

6.7 
What causes Maundertype
Grand Minima? 

6.8 
Where do we go from here? 
7 
Acknowledgement 

References 

Footnotes 

Updates 

Figures 

Tables 