  Interstellar dust is a significant component of matter in the galaxies. The
dust owns its origin and reprocessing in a wide range of astrophysical
environments. In order to understand the origin and evolution of the distinct
types of interstellar dust grains, we have attempted a comprehensive correlated
study of the thermodynamics condensation of dust grains in distinct stellar
environments with the Galactic chemical evolution of the Milky Way Galaxy. The
Galaxy is evolved in terms of elemental evolution resulting from stellar
nucleosynthetic contributions of several generations of stars. Based on the
elemental composition of the evolving Galaxy, the relative abundances of the
major constituents of interstellar dust are assessed. The major aim is to
redistribute the various condensable elements at any epoch during the evolution
of the Galaxy into various grain constituents and understand their abundance
evolution based on a mass-balance formalism. We also performed thermodynamical
equilibrium condensation calculations to understand the stellar origin of
various grain constituents that could carry the isotopic signatures of the
various stellar nucleosynthetic sources. This is perhaps a novel attempt to
estimate the bulk dust mass budget in the evolving Galaxy. The normalized mass
of the Galactic dust is predicted to decrease with the increase in distance
from the Galactic centre. It increases over time. The supernovae SN Ia are
predicted as the most prominent sources of Fe-dust mass, the supernovae SN
II+Ib/c produces oxides and silicate dust mass, and the AGB stars contributes
to carbonaceous dust mass.
