  A fully self-consistent model of the neutron star inner crust based upon
models of the nucleonic equation of state at zero temperature is constructed.
The results nearly match those of previous calculations of the inner crust
given the same input equation of state. The extent to which the uncertainties
in the symmetry energy, the compressibility, and the equation of state of
low-density neutron matter affect the composition of the crust are examined.
The composition and pressure of the crust is sensitive to the description of
low-density neutron matter and the nuclear symmetry energy, and the latter
dependence is non-monotonic, giving larger nuclei for moderate symmetry
energies and smaller nuclei for more extreme symmetry energies. Future nuclear
experiments may help constrain the crust and future astrophysical observations
may constrain the nuclear physics input.
