  We explore neutrino emission from nonrotating, single star models across six
initial metallicities and seventy initial masses from the zero-age main
sequence to the final fate. Overall, across the mass spectrum, we find
metal-poor stellar models tend to have denser, hotter and more massive cores
with lower envelope opacities, larger surface luminosities, and larger
effective temperatures than their metal-rich counterparts. Across the
mass-metallicity plane we identify the sequence (initial CNO $\rightarrow$
$^{14}$N $\rightarrow$ $^{22}$Ne $\rightarrow$ $^{25}$Mg $\rightarrow$
$^{26}$Al $\rightarrow$ $^{26}$Mg $\rightarrow$ $^{30}$P $\rightarrow$
$^{30}$Si) as making primary contributions to the neutrino luminosity at
different phases of evolution. For the low-mass models we find neutrino
emission from the nitrogen flash and thermal pulse phases of evolution depend
strongly on the initial metallicity. For the high-mass models, neutrino
emission at He-core ignition and He-shell burning depends strongly on the
initial metallicity. Anti-neutrino emission during C, Ne, and O burning shows a
strong metallicity dependence with $^{22}$Ne($\alpha$,$n$)$^{25}$Mg providing
much of the neutron excess available for inverse-$\beta$ decays. We integrate
the stellar tracks over an initial mass function and time to investigate the
neutrino emission from a simple stellar population. We find average neutrino
emission from simple stellar populations to be 0.5--1.2 MeV electron neutrinos.
Lower metallicity stellar populations produce slightly larger neutrino
luminosities and average $\beta$ decay energies. This study can provide targets
for neutrino detectors from individual stars and stellar populations. We
provide convenient fitting formulae and open access to the photon and neutrino
tracks for more sophisticated population synthesis models.
