These physical disk models are the solution of two calculations: the first one is the determination
of the detailed vertical structure of the accretion disk taking into account heating
from the stellar radiation and from viscous disipation due to accretion. The second one is
the computation of the emision maps of the disk by solving the transfer equations for thermal and scattered
light in rays parallel to the line of sight and integrate them in solid angle to generate a synthetic
Spectral Energy Distribution. In both computations all parameters are selfconsistently calculated with
the star and disk input parameters.


The models have the following properties:
 The energy is transported by radiation, convection and turbulent flux 
 Heating due to viscous dissipation and stellar flux irradiation. 
 Self consistent irradiation surface with hydrostatic solution to
disk structure. 
.. and have the following assumptions:
 Disc in steady state 
 Geometrically thin 
 viscosity parametrization 
 Dust and gas well mixed 
 Radiation field is supposed to have two main regimes: stellar and disk radiation fields 
 Radiative transfer solved with the two first moments of equation 


A more detailed definition of the models is available in D'Alessio et al.(2004) or in the following presentation.
