  Galactic nuclei, the densest stellar environments in the Universe, exhibit a
complex geometrical structure. The stars orbiting the central supermassive
black hole follow a mass segregated distribution both in the radial distance
from the center and in the inclination angle of the orbital planes. The latter
distribution may represent the equilibrium state of vector resonant relaxation
(VRR). In this paper, we build simple models to understand the equilibrium
distribution found previously in numerical simulations. Using the method of
maximising the total entropy and the quadrupole mean-field approximation, we
determine the equilibrium distribution of axisymmetric two-component
gravitating systems with two distinct masses, semimajor axes, and
eccentricities. We also examine the limiting case when one of the components
dominates over the total energy and angular momentum, approximately acting as a
heat bath, which may represent the surrounding astrophysical environment such
as the tidal perturbation from the galaxy, a massive perturber, a gas torus, or
a nearby stellar system. Remarkably, the bodies above a critical mass in the
subdominant component condense into a disk in a ubiquitous way. We identify the
system parameters where the transition is smooth and where it is discontinuous.
The latter cases exhibit a phase transition between an ordered disk-like state
and a disordered nearly spherical distribution both in the canonical and in the
microcanonical ensembles for these long-range interacting systems.
