  Interstellar dust plays decisive roles in the conversion of neutral to
molecular hydrogen (H_2), the thermodynamical evolution of interstellar medium
(ISM), and the modification of spectral energy distributions (SEDs) of
galaxies. These important roles of dust have not been self-consistently
included in previous numerical simulations of galaxy formation and evolution.
We have therefore developed a new model by which one can investigate whether
and how galaxy formation and evolution can be influenced by dust-related
physical processes such as photo-electric heating, H_2 formation on dust, and
stellar radiation pressure on dust in detail. A novel point of the model is
that different dust species in a galaxy are represented by `live dust'
particles (i.e., not test particles). Therefore, dust particles in a galaxy not
only interact gravitationally with all four components of the galaxy (i.e.,
dark matter, stars, gas, and dust) but also are grown and destroyed through
physical processes of ISM. First we describe a way to include dust-related
physical processes in Nbody+hydrodynamical simulations of galaxy evolution in
detail. Then we show some preliminary results of dust-regulated galaxy
evolution. The preliminary results suggest that the evolution of dust
distributions driven by radiation pressure of stars is very important for the
evolution of star formation rates, chemical abundances, H_2 fractions, and gas
distributions in galaxies.
