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The importance of microphysical inputs from laboratory nuclear experimentsand theoretical nuclear structure calculations in the understanding of the corecollapse dynamics, and the subsequent supernova explosion, is largelyrecognized in the recent literature. In this work, we analyze the impact of themasses of very neutron rich nuclei on the matter composition during collapse,and the corresponding electron capture rate. To this aim, we introduce anempirical modification of the popular Duflo-Zuker mass model to account forpossible shell quenching far from stability, and study the effect of thequenching on the average electron capture rate. We show that the preeminence ofthe $N=50$ and $N=82$ closed shells in the collapse dynamics is considerablydecreased if the shell gaps are reduced in the region of $^{78}$Ni and beyond.As a consequence, local modifications of the overall electron capture rate upto 30\% can be expected, with integrated values strongly dependent on thestiffness of magicity quenching and progenitor mass and potential importantconsequences on the entropy generation, the neutrino emissivity, and the massof the core at bounce. Our work underlines the importance of new experimentalmeasurements in this region of the nuclear chart, the most crucial informationbeing the nuclear mass and the Gamow-Teller strength. Reliable microscopiccalculations of the associated elementary rate, in a wide range of temperaturesand electron densities, optimized on these new empirical information, will beadditionally needed to get quantitative predictions of the collapse dynamics.

Modification of magicity towards the dripline and its impact on electron-capture rates for stellar core-collapse