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Accurate estimate of neutrino energy loss rates are needed for the study ofthe late stages of the stellar evolution, in particular for cooling of neutronstars and white dwarfs. The energy spectra of neutrinos and antineutrinosarriving at the Earth can also provide useful information on the primaryneutrino fluxes as well as neutrino mixing scenario (it is to be noted thatthese supernova neutrinos are emitted after the supernova explosion which is amuch later stage of stellar evolution than that considered in this paper).Recently an improved microscopic calculation of weak-interaction mediated ratesfor iron isotopes was introduced using the proton-neutron quasiparticle randomphase approximation (pn-QRPA) theory. Here I present for the first time thefine-grid calculation of the neutrino and anti-neutrino energy loss rates dueto $^{54,55,56}$Fe in stellar matter. In the core of massive stars isotopes ofiron, $^{54,55,56}$Fe, are considered to be key players in decreasing theelectron-to-baryon ratio ($Y_{e}$) mainly via electron capture on thesenuclide. Core-collapse simulators may find this calculation suitable forinterpolation purposes and for necessary incorporation in the stellar evolutioncodes. The calculated cooling rates are also compared with previouscalculations.

Neutrino and anti-neutrino energy loss rates due to iron isotopes suitable for core-collapse simulations