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