The development of both ground- and space-based techniques for studying the dynamo and reconnection in the local cosmos combined with the development of theoretical/computational models has led to unprecedented progress in the understanding of both of these fundamentally important processes. Nevertheless, understanding naturally occurring dynamos and reconnection processes is complicated because of, for example, the complexity of the geometries, the inhomogeneity of important parameters, and the multiplicity of spatial scales involved. In recent years dedicated laboratory experiments have begun to play an increasingly important role in unraveling some of the important issues on these topics. Laboratory experiments have the advantage over naturally occurring phenomena that parameters can be varied to test ideas about the scaling of phenomena. Laboratory experiments on magnetic reconnection in particular have been constructed at national laboratories and university sites in both the United States and abroad. These experiments are now able to explore magnetic reconnection in both the collisional and collisionless regimes, test ideas about the scaling of the size of the dissipation region with parameters, explore the differences between reconnection with and without a guide field, and study the development of turbulence and its impact on the rate of reconnection. Theoretical modeling has in particular served to catalyze the interaction between laboratory experiments and satellite and other observations by providing testable ideas about the dominant processes that control reconnection. Several laboratory liquid metal dynamo experiments have also been constructed. Flows generated by propellers have been shown to reduce the rate of decay of seed magnetic fields, providing hope that the construction of larger-scale experiments (with larger Reynolds number) will demonstrate self-generation. An experiment that self-generates a seed magnetic field as a result of externally supplied flows would provide a wealth of data for benchmarking theoretical models.

The generation of magnetic fields and their subsequent conversion into plasma kinetic energy have abundant examples throughout the universe. Thus, the creation and annihilation of magnetic fields take place over an enormous range of plasma densities and temperatures. However, in most cases similar physical processes are expected to control the essential dynamics. Solar physics and space physics are in a unique position to advance our understanding of these phenomena because of the accessibility of the Sun and the heliosphere to experimentation.

In the case of the Sun, high-resolution optical measurements can be used to investigate the small-scale fibril structure of the magnetic field and the role of magnetic reconnection in the development of flares and coronal mass ejections. Throughout the heliosphere, and especially at the planets, direct measurements of magnetic and electric fields, plasmas, and energetic particles can be used to test theories of the creation and annihilation of magnetic fields. Thus, the heliosphere is at once the setting for direct investigation of specific processes important to solar system plasmas and a laboratory for the investigation of magnetic-field phenomena important to the broader astrophysical plasma physics program.

Front Matter (R1-R10)

Executive Summary (1-4)

1 Our Local Cosmic Laboratory (5-10)

2 Creation and Annihilation of Magnetic Fields (11-27)

3 Formation of Structures and Transients (28-45)

4 Plasma Interactions (46-56)

5 Explosive Energy Conversion (57-64)

6 Energetic Particle Acceleration (65-76)

7 Concluding Thoughts (77-78)

Appendix A: Statement of Task (79-82)

Appendix B: Study Groups (83-84)

Appendix C: Acronyms and Abbreviations (85-86)