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Neutrino losses from proto-neutron stars play a pivotal role to decide ifthese stars would be crushed into black holes or explode as supernovae. Recentobservations of subluminous Type II-P supernovae (e.g., 2005cs, 2003gd, 1999br,1997D) were able to rejuvenate the interest in 8-10 M$_{\odot}$ stars whichdevelop O+Ne+Mg cores. Simulation results of O+Ne+Mg cores show varying resultsin converting the collapse into an explosion. The neutrino energy loss ratesare important input parameters in core collapse simulations. Proton-neutronquasi-particle random phase approximation (pn-QRPA) theory has been used forcalculation of neutrino energy loss rates due to $^{24}$Mg in stellar matter.The rates are presented on a detailed density-temperature grid suitable forsimulation purposes. The calculated neutrino energy loss rates are enhanced upto more than one order of magnitude compared to the shell model calculationsand favor a lower entropy for the core of these massive stars.

Stellar neutrino energy loss rates due to $^{24}$Mg suitable for O+Ne+Mg core simulations