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 ν, = 0.02398 · L γ, = 9.1795 × 10 31 erg s −1 ) as a normalization, we identify 0.3 MeV electron neutrino emission from helium burning during the helium flash (peak L ν /L ν, 10 4 , flux Φ ν,He flash 170 (10 pc/d) 2 cm −2 s −1 for a star located at a distance of d parsec, timescale 3 days) and the thermal pulse (peak L ν /L ν, 10 9 , flux Φ ν,TP 1.7×10 7 (10 pc/d) 2 cm −2 s −1 , timescale 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.

Lynds 1642 is a small, somewhat insignificant dark cloud centred at 04h33, — 14°20 (1950). On a IIIaJ UKSTU Schmidt plate it may be seen to lie within an approximately circular patch of nebulosity which we believe to be visible by reflection. Its galactic location (l = 210°.9 b = -36°.5) places it beneath the local arm in the direction of Orion and it is likely that it is seen by reflection of the integrated light of the stars in that region of the galaxy.

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