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Multi-energy diffuse neutrino fluxes originating from core-collapse supernovae

Yosuke Ashida

Abstract

Diffuse neutrino fluxes attributed to two different physical processes in core collapse of massive stars are visited with their potentiality of exploring stellar physics more deeply being stressed. In this work, available models of thermal MeV-scale neutrinos produced at the core of collapsing stars and non-thermal high-energy neutrinos emitted from accelerated cosmic rays interacting with circumstellar material are bridged through features of core-collapse supernovae such as progenitor mass and optical properties. The calculated diffuse fluxes are presented with discussion about their detection prospects at neutrino telescopes.

Multi-energy diffuse neutrino fluxes originating from core-collapse supernovae

Abstract

Diffuse neutrino fluxes attributed to two different physical processes in core collapse of massive stars are visited with their potentiality of exploring stellar physics more deeply being stressed. In this work, available models of thermal MeV-scale neutrinos produced at the core of collapsing stars and non-thermal high-energy neutrinos emitted from accelerated cosmic rays interacting with circumstellar material are bridged through features of core-collapse supernovae such as progenitor mass and optical properties. The calculated diffuse fluxes are presented with discussion about their detection prospects at neutrino telescopes.
Paper Structure (10 sections, 6 equations, 2 figures, 1 table)

This paper contains 10 sections, 6 equations, 2 figures, 1 table.

Table of Contents

  1. Introduction
  2. Supernova classification
  3. Neutrino emission
  4. Neutrinos from thermal process at stellar core
  5. Neutrinos from pp interactions in outer region
  6. Diffuse neutrino flux
  7. Diffuse flux of thermal SN neutrinos (DSNB)
  8. Diffuse flux of non-thermal CSM-origin SN neutrinos
  9. Discussion
  10. Conclusion

Figures (2)

  • Figure 1: Calculated DSNB $\bar{\nu}_e$ flux in comparison with experimental upper limits from Super-Kamiokande 2021PhRvD.104l2002A2025arXiv251102222A and KamLAND 2022ApJ...925...14A. Contributions from the CNS and HNS cases with $f_{\rm HNS}=0.24$, and their sum are shown. The bands cover different choices of the nuclear EOS (LS220, Shen, or Togashi) and neutrino mass ordering (NMO or IMO).
  • Figure 2: Calculated diffuse high-energy SN neutrino flux ($\nu_e + \bar{\nu}_e + \nu_\mu + \bar{\nu}_\mu + \nu_\tau + \bar{\nu}_\tau$) in comparison with the measured diffuse astrophysical neutrino flux in a recent IceCube analysis using starting track events (ESTES) 2024PhRvD.110b2001A. Contributions from each SN type and their sum are shown. The bands cover the different spectral indices of the parent cosmic ray flux ($2.0 \leq s \leq 2.2$).