  We explore the evolution of a select grid of solar metallicity stellar models
from their pre-main sequence phase to near their final fates in a neutrino
Hertzsprung-Russell diagram, where the neutrino luminosity replaces the
traditional photon luminosity. Using a calibrated \MESA\ solar model for the
solar neutrino luminosity ($L_{\nu,\odot}$ = 0.02398 $\cdot$ $L_{\gamma,\odot}$
= 9.1795 $\times$ 10$^{31}$ erg s$^{-1}$) as a normalization, we identify
$\simeq$ 0.3 MeV electron neutrino emission from helium burning during the
helium flash (peak $L_{\nu} / L_{\nu,\odot} \simeq$ 10$^4$, flux $\Phi_{\nu,
{\rm He \ flash}} \simeq$ 170 (10 pc/$d$)$^{2}$ cm$^{-2}$ s$^{-1}$ for a star
located at a distance of $d$ parsec, timescale $\simeq$ 3 days) and the thermal
pulse (peak $L_{\nu} / L_{\nu,\odot} \simeq$ 10$^9$, flux $\Phi_{\nu, {\rm TP}}
\simeq$ 1.7$\times$10$^7$ (10 pc/$d$)$^{2}$ cm$^{-2}$ s$^{-1}$, timescale
$\simeq$ 0.1 yr) phases of evolution in low mass stars as potential probes for
stellar neutrino astronomy. We also delineate the contribution of neutrinos
from nuclear reactions and thermal processes to the total neutrino loss along
the stellar tracks in a neutrino Hertzsprung-Russell diagram. We find, broadly
but with exceptions, that neutrinos from nuclear reactions dominate whenever
hydrogen and helium burn, and that neutrinos from thermal processes dominate
otherwise.
