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Our previous investigation of neutron-star crusts, based on the functionalBSk24, led to a substantial reduction of the pasta mantle when Strutinskyintegral and pairing corrections were added on top of the fourth-order extendedThomas-Fermi method (ETF). Here, our earlier calculations are widened to alarger set of functionals within the same family, and we find that themicroscopic corrections weaken significantly the influence of the symmetryenergy. In particular, the correlation observed at the pure ETF level betweenthe density for the onset of pasta formation and the symmetry energy vanishes,not only for the $L$ coefficient but also for the symmetry-energy values at therelevant densities. Moreover, the inclusion of microscopic corrections resultsin a much lower abundance of pasta for all functionals.

Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. IV. Role of the symmetry energy in pasta phases