  Core-collapse supernovae are considered to be important contributors to the
primitive dust enrichment of the interstellar medium in the high-redshift
universe. Theoretical models of dust formation in stellar explosions have so
far provided controversial results and a generally poor fit to the observations
of dust formation in local supernovae. We present a new methodology for the
calculation of carbonaceous dust formation in young supernova remnants. Our new
technique uses both the nucleation theory and a chemical reaction network to
allow us to compute the dust growth beyond the molecular level as well as to
consider chemical erosion of the forming grains. We find that carbonaceous dust
forms efficiently in the core of the ejecta, but takes several years to
condensate, longer than previously estimated. It forms unevenly and remains
concentrated in the inner part of the remnant. These results support the role
of core-collapse supernovae as dust factories and provide new insight on the
observations of SN 1987A, in which large amounts of dust have been detected to
form on a timescale of years after core collapse.
