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Article Contents

ABSTRACT

1.INTRODUCTION

2.INTERPRETATION OF RADIO OBSERVATIONS

2.1.Field Strength Estimates

2.2.Large-Scale Field Patterns

2.3.Small-Scale Field Structures

2.4.Comparison with Optical Polarization Data

3.MAGNETIC FIELDS IN SPIRAL GALAXIES

3.1.Field Strengths

3.2.M31: The Nearly Perfect Magnetic Torus

3.3.Density-Wave Galaxies

3.4.IC 342 and NGC 6946: Magnetic Spiral Arms

3.5.ASS, BSS, or What?

3.6.Magnetic Fields in Galactic Halos

3.7.Magnetic Fields in High-Redshift Galaxies

3.8.The Milky Way

4.GALACTIC DYNAMO THEORY

4.1.Random Magnetic Fields

4.2.Large-Scale Fields

4.3.Treatment of Galactic Turbulence

4.4.Basic Galactic Dynamo Models

4.5.The Quenching Problem

5.ORIGIN OF GALACTIC MAGNETIC FIELDS

5.1.Cosmological Magnetic Fields

5.2.The Primordial Origin of Galactic Magnetic Fields

5.3.The Dynamo Origin of Magnetic Field

6.EFFECTS OF THE DYNAMO ENVIRONMENT

6.1.Starbursts

6.2.Galactic Encounters

6.3.Parametric Resonance with Spiral Arms

6.4.Contrast Structures

6.5.The Influence of Magnetic Fields on the Galactic Disk

7.MAGNETIC FIELDS IN HALOS

7.1.In Situ Generation

7.2.Transport Out of the Disk

8.MAGNETIC FIELD MODELS

8.1.The Parity

8.2.Large-Scale Azimuthal Patterns

8.3.Spiral Field Lines and Pitch Angles

8.4.Spiral Arms and Magnetic Fields

8.5.Dynamo Models for Individual Galaxies

9.LAST WORDS

REFERENCES