  In this paper, extending the investigation developed in an earlier paper
(Cremaschini et al., 2008), we pose the problem of the kinetic description of
gravitational Hall-MHD equilibria which may arise in accretion disks (AD)
plasmas close to compact objects. When intense EM and gravitational fields,
generated by the central object, are present, a convenient approach can be
achieved in the context of the Vlasov-Maxwell description. In this paper the
investigation is focused primarily on the following two aspects:
  1) the formulation of the kinetic treatment of G-Hall-MHD equilibria. Based
on the identification of the relevant first integrals of motion, we show that
an explicit representation can be given for the equilibrium kinetic
distribution function. For each species this is represented as a superposition
of suitable generalized Maxwellian distributions;
  2) the determination of the constraints to be placed on the fluid fields for
the existence of the kinetic equilibria. In particular, this permits a unique
determination of the functional form of the species number densities and of the
fluid partial pressures, in terms of suitably prescribed flux functions.
