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Neutrino losses play a crucial role in the evolution of massive stars. Westudy the neutrino luminosity of stars ranging from 20 to 90 M_{\odot} fromZero Age Main Sequence (ZAMS) to Fe Core Collapse (FeCC) with differentrotation and metallicity in a neutrino Hertzsprung-Russell diagram. In oursimulations, we consider {\omega}/{\omega}crit = 0 and 0.7 to representnon-rotation and high rotation, respectively, and set the metallicities to0.014, 0.001, and 0.0001. During hydrogen burning stages, neutrino luminosityprimarily originates from CNO cycle, and increases with higher stellar masswhile decreasing with increasing metallicity. For the high metallicity models(Z = 0.014) during the helium burning stage, the reduction of the hydrogenenvelope caused by a larger mass loss rate leads to a gradual decrease inneutrino luminosity. The rapid rotation results in extra mixing inside massivestars, which increases the neutrino luminosity during main sequence (MS), whiledecreases the neutrino luminosity during helium burning phase. Simultaneously,the rapid rotation also increases CO core mass, which enhances the neutrinoluminosity during C and O burning phase. We also investigate the effect ofneutrino magnetic moment (NMM) on the massive stars. We find that the energyloss caused by the NMM does not have effects on the evolutionary destiny ofmassive stars, and it does not significant change the compactness at the timeof Fe core collapse.

Evolutionary tracks of massive stars with different rotation and metallicity in neutrino H-R diagram