  We analyze a two dimensional viscoresistive magnetohydrodynamical (MHD) model
for a thin accretion disk which reconciles the crystalline structure outlined
in [Coppi(2005), Coppi and Rousseau(2006)] with real microscopic and
macroscopic features of astrophysical accreting systems. In particular, we
consider small dissipative effects (viscosity and resistivity, characterized by
a magnetic Prandtl number of order unity), poloidal matter fluxes and a
toroidal component of the magnetic field. These new ingredients allow us to set
up the full equilibrium profile including the azimuthal component of the
momentum conservation equation and the electron force balance relation. These
two additional equations, which were identically satisfied in the original
model, permit us to deal with non-zero radial and vertical matter fluxes, and
the solution we construct for the global equilibrium system provides a full
description of the radial and vertical dependence within the plasma disk. The
main issue of our analysis is outlining a modulation of the matter distribution
in the disk which corresponds to the formation of a ring-like sequence, here
associated with a corresponding radial oscillation of the matter flux.
