  We present a first attempt to construct an analytic model for a clumped gas
and dust disk and apply it to the Galactic Centre. The clumps are described as
isothermal spheres partially ionized by the external UV radiation field. The
disk structure formed by the clouds is described as a quasi standard continuous
accretion disk using adequately averaged parameters of the discrete cloud
model. The viscosity in the Circumnuclear Disk is due to partially inelastic
cloud-cloud collisions. We find two different solutions for the set of
equations corresponding to two stable cloud regimes: (i) the observed molecular
clouds and (ii) much lighter and smaller clouds which correspond to the
stripped cores of the observed clouds. It is shown that the resulting physical
characteristics of the heavy clouds and the disk are in very good agreement
with all comparable observations at multiple wavelengths. A mass accretion rate
of approx. 10^-4 M_solar/yr for the isolated Circumnuclear Disk is inferred. We
propose that the Circumnuclear Disk has a much longer lifetime (approx. 10^7
yr) than previously assumed.
