Epilogue

There are now several types of relativistic flows in astrophysical settings. The foremost examples are jets and disks orbiting spinning black holes, pulsar winds and gamma ray bursts. As discussed at this meeting, these flows exhibit unusual kinematic and dynamical properties, that distinguish them from non-relativistic flows. It is possible that all collimated outflows are essentially hydromagnetic or electromagnetic. Future study of relativistic flows will rely heavily on numerical experiments. Model relativistic flows provide a basis for carrying out secondary studies of the underlying plasma physics, particle acceleration, magnetic field amplification and the emission and transfer of radiation, particularly at shock fronts. Some current opportunities in observation, phenomenology and theory are briefly suggested.