Numerical experiments on simple or symmetric ejections of massive bodies from the nucleus of a disk of stars are presented. The ejected masses range from 0.04 to 0.1 of the total mass. Either spiral features or a barred structure appear but do not last for a long time. Material arms start leading and become trailing.

Relativistic stellar-dynamical systems and their possible occurrence in nature are discussed. Features of the equilibrium models that have been constructed for spherical star clusters in general relativity are delineated. The results of studies of the stability of relativistic spherical clusters are reviewed. It is noted that the results, while not conclusive, indicate that realistic spherical clusters are stable against gravitational collapse if their central redshifts zc ≲ 0.55 and unstable if zc ≳ 0.55. More work is needed on this and other problems.

The analytic aspects of the Campbell-Hénon method of concentric spherical shells are generalized for application to relativistic spherically symmetric star clusters.

One of the important jobs of scientists is to formulate new laws and principles, and I have attempted to summarise those we have learnt in this most enjoyable and fruitful symposium in the laws stated below. However, recognising that laws derived from stellar dynamics may lead to important discoveries in other fields, I have translated these laws into the language of sociology. The key concept of hard and soft binaries has been introduced into stellar dynamics by Heggie. If at some point in a stellar system is defined to be then Heggie defines a soft binary to be one whose internal energy has β|ε| < 1 and a hard binary to be one with β|ε| > 1. Heggie's laws cover the interaction of these binaries with the field stars and his first basic discovery is that on interacting with this society hard binaries become harder while soft binaries become softer and may even cease to be binaries at all. The same may be true of criminals in their interaction with society.