Multi-Messenger Signals from Stellar Evolution

Stars generate a variety of multi-messenger signals throughout their evolution. They radiate photons from their stellar surface, neutrinos from their interior, and recently-discovered gravitational waves during binary mergers. These signals give us important clues about the composition, nuclear physics, and energy transport in stellar interiors, enabling us to constrain the efficiency of convection, strength of nuclear reactions, and the ultimate structure of white dwarf and pre-supernova stars. In this thesis, I focus on analyzing the multi-messenger signals produced during or as a result of stellar evolution. I evolve thousands of stellar models of low-mass and high-mass stars to their final fate and explore how global features of stellar evolution are reflected in their multi-messenger signals. I present a novel method for analyzing stellar neutrino emission in a neutrino Hertzsprung-Russell diagram. I then discuss neutrino emissions from stars of all masses and metallicities to provide stellar targets for current and forthcoming neutrino detectors. I also discuss the evolution of the most massive stars which result in pair-instability supernovae and make predictions for the black hole (BH) mass spectrum. These predictions are currently being probed with gravitational wave detections of merging binary BHs by the LIGO/VIRGO/KAGRA collaboration. I then show how these gravitational wave signals can be used to constrain the most uncertain nuclear reaction rates in all of astrophysics: the 12C(α,γ)16O and triple-α helium burning nuclear reactions which set the C and O composition of the cosmos.