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On Stellar Evolution In A Neutrino Hertzsprung-Russell Diagram

Published onJun 01, 2020
On Stellar Evolution In A Neutrino Hertzsprung-Russell Diagram

We explore the evolution of a select grid of solar metallicity stellar mod-els 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 (Lν, = 0.02398 · Lγ,⊙ = 9.1795×1031 erg s−1) as a normalization, we identify ≃ 0.3 MeV electron neutrino emission from helium burning during the helium flash (peak Lν/Lν,⊙ ≃ 104, flux Φν,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 Lν/Lν,⊙ ≃ 109, flux Φν,TP ≃ 1.7×107 (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.

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