In magnetorotational stellar collapses, neutrinos undergo resonant flavor conversion in matter plus magnetic-moment-driven chirality flipping for Majorana neutrinos, producing orientation-dependent event rates at detectors that peak 400-600 ms after bounce.
What can be learned from a future supernova neutrino detection?
6 Pith papers cite this work. Polarity classification is still indexing.
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abstract
This year marks the thirtieth anniversary of the only supernova from which we have detected neutrinos - SN 1987A. The twenty or so neutrinos that were detected were mined to great depth in order to determine the events that occurred in the explosion and to place limits upon all manner of neutrino properties. Since 1987 the scale and sensitivity of the detectors capable of identifying neutrinos from a Galactic supernova have grown considerably so that current generation detectors are capable of detecting of order ten thousand neutrinos for a supernova at the Galactic Center. Next generation detectors will increase that yield by another order of magnitude. Simultaneous with the growth of neutrino detection capability, our understanding of how massive stars explode and how the neutrino interacts with hot and dense matter has also increased by a tremendous degree. The neutrino signal will contain much information on all manner of physics of interest to a wide community. In this review we describe the expected features of the neutrino signal, the detectors which will detect it, and the signatures one might try to look for in order to get at these physics.
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Models scalar-mediated νSI on the DSNB in a full three-flavor PMNS framework for four coupling structures and projects 3σ sensitivities at JUNO, Hyper-Kamiokande-Gd, and DUNE reaching g∼10^{-8} for m_ϕ∼100-300 eV.
The helium flash produces a neutrino burst with a 1.7 MeV line detectable up to almost 3 pc in future facilities, but asteroseismology remains the practical probe for now.
Joint analysis of neutrino detectors and CMB observables can constrain dark matter annihilation into neutrinos for MeV-GeV masses.
Hybrid HF-CRPA calculations predict lower allowed cross sections for charged-current ν_e on 40Ar at low energies, leading to ~20% fewer events in DUNE for a galactic supernova burst than the prior MARLEY model.
ESSnuSB far detector shows varying event rates across supernova models and potential to distinguish them depending on distance, systematics, and efficiency.
citing papers explorer
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Study of Supernova Neutrinos at ESSnuSB
ESSnuSB far detector shows varying event rates across supernova models and potential to distinguish them depending on distance, systematics, and efficiency.