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Accurate estimate of the neutrino cooling rates is required in order to studythe various stages of stellar evolution of massive stars. Neutrino losses fromproto-neutron stars play a crucial role in deciding whether these stars wouldbe crushed into black holes or explode as supernovae. Both pure leptonic andweak-interaction processes contribute to the neutrino energy losses in stellarmatter. At low temperatures and densities, characteristic of the early phase ofpresupernova evolution, cooling through neutrinos produced via theweak-interaction is important. Proton-neutron quasi-particle random phaseapproximation (pn-QRPA) theory has recently being used for calculation ofstellar weak-interaction rates of $fp$-shell nuclide with success. Thelepton-to-baryon ratio ($Y_{e}$) during early phases of stellar evolution ofmassive stars changes substantially alone due to electron captures on$^{56}$Ni. The stellar matter is transparent to the neutrinos produced duringthe presupernova evolution of massive stars. These neutrinos escape the siteand assist the stellar core in maintaining a lower entropy. Here I present theexpanded calculation of weak-interaction mediated neutrino and antineutrinocooling rates due to $^{56}$Ni in stellar matter using the pn-QRPA theory. Thisdetailed scale is appropriate for interpolation purposes and of greater utilityfor simulation codes. The calculated rates are compared against earliercalculations. During the relevant temperature and density regions of stellarmatter the reported rates show little differences with the shell model ratesand might contribute in fine-tuning of the lepton-to-baryon ratio during thepresupernova phases of stellar evolution of massive stars.

Expanded calculation of weak-interaction mediated neutrino cooling rates due to $^{56}$Ni in stellar matter