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Electron captures on nuclei play an important role in the dynamics of thecollapsing core of a massive star that leads to a supernova explosion. Recentcalculations of these capture rates were based on microscopic models whichaccount for relevant degrees of freedom. Due to computational restrictions suchcalculations were limited to a modest number of nuclei, mainly in the massrange A=45-110. Recent supernova simulations show that this pool of nuclei,however, omits the very neutron-rich and heavy nuclei which dominate thenuclear composition during the last phase of the collapse before neutrinotrapping. Assuming that the composition is given by Nuclear StatisticalEquilibrium we present here electron capture rates for collapse conditionsderived from individual rates for roughly 2700 individual nuclei. For thosenuclei which dominate in the early stage of the collapse, the individual ratesare derived within the framework of microscopic models, while for the nucleiwhich dominate at high densities we have derived the rates based on the RandomPhase Approximation with a global parametrization of the single particleoccupation numbers. In addition, we have improved previous rate evaluations byproperly including screening corrections to the reaction rates into account.

Improved estimate of electron capture rates on nuclei during stellar core collapse