  We postulate that most stars are born in aggregates of binary systems which
are dynamically equivalent to the `dominant mode cluster'. The initial binary
orbits are consitent with pre-main sequence data. Stellar masses are paired at
random from the KTG(1.3) mass function. We develop a simple model which
establishes the observed correlations between eccentricity, mass ratio and
period. Stimulated evolution of orbital parameters within the cluster places a
few per cent of all orbits into the eigenevolution region of the eccentricity-
period diagram. Observations should reveal the odd binary with eccentric orbits
at periods smaller than the circularisation cutoff period. We show that the
birth eccentricity distribution must be approximately dynamically relaxed
because stimulated evolution in the dominant mode cluster cannot sufficiently
thermalise a significantly different distribution. After disintegration of the
dominant mode cluster we have a proportion of binaries which compares
favourably with the observed proportion. The shape of the period distribution
agrees well with the observed distribution. The mass-ratio distribution of G
dwarf binaries is depleted at small mass ratios and has the shape of the main
sequence distribution. We predict and tabulate the mass ratio distribution for
main sequence binaries with a primary star less massive than $1.1\,M_\odot$.
Our model Galactic field stellar population has a binary proportion among G-,
K- and M-dwarfs in good agreement with the observational data. Too few triple
and quadruple systems form by capture to account for the number of observed
systems. We compare the specific angular momentum distribution of our initial
binary star population with the observed distribution of specific angular
momenta of molecular cloud cores.
