describe the three major goals for the next five years, the
tasks to accomplish these goals, and the tasks with key persons
and approximate time scales.
1. Understand generic
properties of nonlinear MHD dynamos. What determines the
nonlinear saturation? What is the structure of dynamo fields
at small magnetic Prandtl number? How are large scale fields
generated by inverse cascades? Why is the alpha effect strong
in the RFP and weak in numerical simulations aimed at astrophysics?
2. Develop a self-consistent
computational model for the “solar dynamo”. Build a code
that integrates multiple physical processes in spherical and
cylindrical geometry. Focus understanding origin of the large-scale
magnetic field. Compare with solar observations, and with available
liquid metal experiments.
3. Understand the dynamics
of dynamo effects beyond MHD, and their relevance to astrophysics
and experiments. Under what conditions are different dynamo
effect large? What is the relation of reconnection layer physics
to dynamos? Which dynamo effects dominates in experiment? Are
there important astrophysical situations for which non-MHD dynamo
effects are significant?