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