  The topic of the present study is combining a dynamic model of a
protoplanetary disk with the computations of radiation transfer for obtaining
synthetic spectra and disk images suitable for immediate comparison of the
model with observations. Evolution of the disk was computed using the FEOSAD
hydrodynamic model, which includes a self-consistent calculation of the
dynamics of dust and gas in the 2D thin disk approximation. Radiation transfer
was simulated by the open code RADMC-3D. Three phases of disk evolution were
considered: a young gravitationally unstable disk, a disk during an accretion
luminosity burst, and an evolved disk. For these stages, the influence of
various processes upon the disk's thermal structure was analyzed, as well as
the differences between the temperatures obtained in the initial dynamic model
and in the model with a detailed calculation of the radiation transfer. It is
shown that viscous heating in the inner regions and adiabatic heating in the
disk spirals can be important sources of heating. On the basis of the
calculated spectral energy distributions, using SED-fitter software package
used for the observations, physical parameters of the model disks were
reconstructed. A significant spread between reconstructed parameters and
initial characteristics of the disk indicates verification necessity of the
models within the framework of spatially resolved observations of disks in the
different spectral ranges
