  We explore the nucleosynthesis trends from two mechanisms during freeze-out
expansions in core-collapse supernovae. The first mechanism is related to the
convection and instabilities within homogeneous stellar progenitor matter that
is accreted through the supernova shock. The second mechanism is related to the
impact of the supersonic wind termination shock (reverse shock) within the
tumultuous inner regions of the ejecta above the proto-neutron star. Our
results suggest that isotopes in the mass range 12<=A<=122 that are produced
during the freeze-out expansions may be classified in two families. The
isotopes of the first family manifest a common mass fraction evolutionary
profile, whose specific shape per isotope depends on the characteristic
transition between two equilibrium states (equilibrium state transition) during
each type of freeze-out expansion. The first family includes the majority of
isotopes in this mass range. The second family is limited to magic nuclei and
isotopes in their locality, which do not sustain any transition, become nuclear
flow hubs, and dominate the final composition. We use exponential and power-law
adiabatic profiles to identify dynamic large-scale and small-scale equilibrium
patterns among nuclear reactions. (truncated abstract) In addition, we
introduce non-monotonic parameterized profiles to probe the impact of the
reverse shock and multi-dimensional explosion asymmetries on nucleosynthesis.
Cases are shown in which the non-monotonic profiles favor the production of
radioactivities. Non-monotonic freeze-out profiles involve longer
non-equilibrium nucleosynthesis intervals compared with the exponential and
power-law profiles, resulting in mass fraction trends and yield distributions
that may not be achieved by the monotonic freeze-out profiles.
