  Interiors of neutron stars are ultra-dense and may contain a core of
deconfined quark matter. Such a core connects to the outer layers smoothly or
through a sharp microscopic interface or through an intermediate macroscopic
layer of inhomogeneous mixed phases, which is globally neutral but locally
contains electrically charged domains. Here I employ a nucleon-meson model
under neutron star conditions that shows a first-order chiral phase transition
at large densities. In the vicinity of this chiral transition I calculate the
free energies of various mixed phases - different 'pasta structures' - in the
Wigner-Seitz approximation. Crucially, chirally broken nuclear matter and the
approximately chirally symmetric phase (loosely interpreted as quark matter)
are treated on the same footing. This allows me to compute the interface
profiles of bubbles, rods, and slabs fully consistently, taking into account
electromagnetic screening effects and without needing the surface tension as an
input. I find that the full numerical results tend to disfavor mixed phases
compared to a simple step-like approximation used frequently in the literature
and that the predominantly favored pasta structure consists of slabs with a
surface tension $\Sigma \simeq 6\, {\rm MeV}/{\rm fm}^2$.
