  We present new results for ground-state candidate energies of Mg-rich olivine
(MRO) clusters and use the binding energies of these clusters to determine
their nucleation rates in stellar outflows, with particular interest in the en-
vironments of core-collapse supernovae (CCSNe). Low-lying structures of
clusters (Mg2SiO4)n 2 \le n \le 13 are determined from a modified minima
hopping algorithm using an empirical silicate potential in the Buckingham form.
These configurations are further refined and optimized using the den- sity
functional theory code Quantum Espresso. Utilizing atomistic nucleation theory,
we determine the critical size and nucleation rates of these clusters. We find
that configurations and binding energies in this regime are very dis- similar
from those of the bulk lattice. Clusters grow with SiO_4-MgO layering and
exhibit only global, rather than local, symmetries. When compared to classical
nucleation theory we find suppressed nucleation rates at most temperatures and
pressures, with enhanced nucleation rates at very large pressures. This implies
a slower progression of silicate dust formation in stellar environments than
previously assumed.
