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We generalize our earlier work on neutron stars (arXiv:1903.04981), whichassumed spherical Wigner-Seitz cells in the inner crust, to admit thepossibility of pasta phases, i.e., non-spherical cell shapes. Full fourth-orderextended Thomas-Fermi calculations using the density functional BSk24 areperformed for cylindrical and plate-like cells. Unlike in our spherical-cellcalculations, we do not include shell and pairing corrections, but there aregrounds for expecting these corrections for pasta to be significantly smaller.It is therefore meaningful to compare the ETF pasta results with the fullspherical-cell results, i.e., with shell and pairing corrections included.However, in view of the many previous studies in which shell and pairingcorrections were omitted entirely, it is of interest to compare our pastaresults with the ETF part of the corresponding spherical calculations. Makingthis latter comparison we find that as the density increases the cell shapespass through the usual sequence sphere $\to$ cylinder $\to$ plate before thetransition to the homogeneous core. The filling fractions found at the phasetransitions are in close agreement with expectations based on the liquid-dropmodel. On the other hand, when we compare with the full spherical-cell results,we find the sequence to be sphere $\to$ cylinder $\to$ sphere $\to$ cylinder$\to$ plate. In neither case do any "inverted", i.e., bubble-like,configurations appear. We provide accurate fitting formulas to all ouressential numerical results for each of the three phases, designed especiallyfor the density range where the nonspherical shapes are expected, which enableone to capture not only the general behavior of the fitted functions, but alsothe differences between them in different phases.

Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. II. Pasta phases in semi-classical approximation