Neutrino Energy Loss Rates due to [sup 54,55,56]Fe in Stellar Environment

Neutrino energy loss rates are required as a key nuclear physics input parameter in the simulation codes of core‐collapse supernovae of massive stars. The weak interaction rates due to isotopes of iron, 54,55,56Fe, are considered to play an important role during the presupernova evolution of massive stars. Proton‐neutron quasi‐particle random phase approximation (pn‐QRPA) theory has recently being used for a microscopic calculation of stellar weak interaction rates of iron isotopes with success. The calculation of neutrino energy loss rates due to 54,55,56Fe is presented along with a comparison with large scale shell model results.