  We study the interactions and the conditions for the equilibrium of forces
between generic non-rotating black holes of the Einstein-Maxwell-Dilaton (EMD)
theory. We study known (and some new) solutions of the time-symmetric
initial-data problem escribing an arbitrary number of those black holes, some
of them with primary scalar hair. We show how one can distinguish between
initial data corresponding to dynamical situations in which the black holes
(one or many) are not in equilibrium and initial data which are just
constant-time slices of a static solution of the full equations of motion
describing static black holes using (self-)interaction energies. For a single
black hole, non-vanishing self-interaction energy is always related to primary
scalar hair and to a dynamical black hole. Removing the self-interaction
energies in multi-center solutions we get interaction energies related to the
attractive and repulsive forces acting on the black holes. As shown by Brill
and Lindquist, for widely separated black holes, these take the standard
Newtonian and Coulombian forms plus an additional interaction term associated
with the scalar charges which is attractive for like charges.
