Presupernova neutrinos: realistic emissivities from stellar evolution

Abstract

We present a new calculation of neutrino emissivities and energy spectra from a massive star going through the advanced stages of nuclear burning (presupernova) in the months before becoming a supernova. The contributions from beta decay and electron capture, pair annihilation, plasmon decay, and the photoneutrino process are modeled in detail, using updated tabulated nuclear rates. We also use realistic conditions of temperature, density, electron fraction and nuclear isotopic composition of the star from the state of the art stellar evolution code MESA. Results are presented for a set of progenitor stars with mass between 15 $M_{\odot }$ and 30 $M_{\odot }$. It is found that beta processes contribute substantially to the neutrino emissivity above realistic detection thresholds of few MeV, at selected positions and times in the evolution of the star.

17 pages, 6 figures

References in corpus (12)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
• Neutrino Physics with JUNO
• The Landscape of the Neutrino Mechanism of Core-Collapse Supernovae: Neutron Star and Black Hole Mass Functions, Explosion Energies and Nickel Yields
• On Variations Of Pre-Supernova Model Properties
• Detection possibility of the pair-annihilation neutrinos from the neutrino-cooled pre-supernova star
• The Sensitivity of Core-Collapse Supernovae to Nuclear Electron Capture
• KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars
• Presupernova neutrino events relating to the final evolution of massive stars
• Long-Baseline Neutrino Facility (LBNF) and Deep Underground Neutrino Experiment (DUNE) Conceptual Design Report Volume 3: Long-Baseline Neutrino Facility for DUNE June 24, 2015
• Nuclear Statistical Equilibrium neutrino spectrum
• Plasmaneutrino spectrum

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