  Baryonic matter close to the saturation density is very likely to present
complex inhomogeneous structures collectively known under the name of pasta
phase. At finite temperature, the different geometric structures are expected
to coexist, with potential consequences on the neutron star crust conductivity
and neutrino transport in supernova matter. In the framework of a statistical
multi-component approach, we calculate the composition of matter in the pasta
phase considering density, proton fraction, and geometry fluctuations. Using a
realistic energy functional from relativistic mean field theory and a
temperature and isospin dependent surface tension fitted from Thomas-Fermi
calculations, we show that different geometries can coexist in a large fraction
of the pasta phase, down to temperatures of the order of the crystallization
temperature of the neutron star crust. Quantitative estimates of the charge
fluctuations are given.
