  We present a new iterative method for constructing equilibrium phase models
of stellar systems. Importantly, this method can provide phase models with
arbitrary mass distributions. The method is based on the following principle.
Our task is to generate an equilibrium N-body system with a given mass
distribution. For this purpose, we let the system reach equilibrium through its
dynamical evolution. During this evolution we hold mass distribution in this
system. This principle is realized in our method by means of an iterative
procedure. We have used our method to construct a phase model of the disc of
our Galaxy. In our method, we use the mass distribution in the Galaxy as input
data. Here we used two Galactic density models (suggested by Flynn,
Sommer-Larsen and Christensen and by Dehnen and Binney). For a fixed-mass model
of the Galaxy we can construct a one-parameter family of equilibrium models of
the Galactic disc. We can, however, choose a unique model using local kinematic
parameters that are known from Hipparcos data. We show that the phase models
constructed using our method are close to equilibrium. The problem of
uniqueness for our models is discussed, and we discuss some further
applications of our method.
