Evolution of interstellar dust

The composition, origins, and evolution of interstellar dust (ISD) are examined, reviewing the results of recent observational and theoretical investigations. Topics discussed include amorphous and polycrystalline structures; the relationship between amorphous C, graphite, and polycyclic aromatic hydrocarbons; observational techniques for determining ISD structure and composition; ISD formation in outflows from late-type giants, planetary nebulae, and novae; destruction of ISD by shocks; the formation of ISD in the ISM; and the relationship between ISD and interplanetary dust. IR spectroscopy of molecular ices and icy grain mantles is considered in detail, and it is shown that typical grain mantles consist of a 1/0.6/0.05/0.05 mixture of H2O, CH3OH, CO, and NH3.