  DUSTY solves the problem of radiation transport in a dusty environment. The
code can handle both spherical and planar geometries. The user specifies the
properties of the radiation source and dusty region, and the code calculates
the dust temperature distribution and the radiation field in it. The solution
method is based on a self-consistent equation for the radiative energy density,
including dust scattering, absorption and emission, and does not introduce any
approximations. The solution is exact to within the specified numerical
accuracy.
  DUSTY has built in optical properties for the most common types of
astronomical dust and comes with a library for many other grains. It supports
various analytical forms for the density distribution, and can perform a full
dynamical calculation for radiatively driven winds around AGB stars. The
spectral energy distribution of the source can be specified analytically as
either Planckian or broken power-law. In addition, arbitrary dust optical
properties, density distributions and external radiation can be entered in user
supplied files. Furthermore, the wavelength grid can be modified to accommodate
spectral features. A single DUSTY run can process an unlimited number of
models, with each input set producing a run of optical depths, as specified.
The user controls the detail level of the output, which can include both
spectral and imaging properties as well as other quantities of interest.
