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.
Core-collapse supernova neutrino emission and detection informed by state-of-the-art three-dimensional numerical models
3 Pith papers cite this work. Polarity classification is still indexing.
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abstract
Based on our recent three-dimensional core-collapse supernova (CCSN) simulations including both exploding and non-exploding models, we study the detailed neutrino signals in representative terrestrial neutrino observatories, Super-Kamiokande (Hyper-Kamiokande), DUNE, JUNO, and IceCube. We find that the physical origin of difference in the neutrino signals between 1D and 3D is mainly proto-neutron-star (PNS) convection. We study the temporal and angular variations of the neutrino signals and discuss the detectability of the time variations driven by the spiral Standing Accretion Shock Instability (spiral SASI) when it emerges for non-exploding models. In addition, we determine that there can be a large angular asymmetry in the event rate ($\gtrsim 50 \%$), but that the time-integrated signal has a relatively modest asymmetry ($\lesssim 20 \%$). Both features are associated with the lepton-number emission self-sustained asymmetry (LESA) and the spiral SASI. Moreover, our analysis suggests that there is an interesting correlation between the total neutrino energy (TONE) and the cumulative number of neutrino events in each detector, a correlation that can facilitate data analyses of real observations. We demonstrate the retrieval of neutrino energy spectra for all flavors of neutrino by applying a novel spectrum reconstruction technique to the data from multiple detectors. We find that this new method is capable of estimating the TONE within the error of $\sim$20\% if the distance to the CCSN is $\lesssim 6$ kpc.
years
2026 3representative citing papers
For a low-mass CCSN progenitor, rotation alone weakly and non-monotonically affects explosion energy and observables; only the fastest spin yields T/|W| spiral modes and spin-kick alignment, with core spin amplified by ~4000.
A parametrization of SASI is introduced that allows IceCube to identify the instability epoch and reconstruct its frequency, peak time, amplitude, and duration from Galactic supernova neutrino signals at sub-percent to ten-percent precision.
citing papers explorer
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Matter- and magnetically-driven flavor conversion of neutrinos in magnetorotational collapses
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.
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Effects of Rotation on 3D Core-Collapse Supernova Models for Low-Mass Progenitors
For a low-mass CCSN progenitor, rotation alone weakly and non-monotonically affects explosion energy and observables; only the fastest spin yields T/|W| spiral modes and spin-kick alignment, with core spin amplified by ~4000.
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Parameterizing the Standing Accretion Shock Instability for Inference with Galactic Supernova Neutrino Signals at IceCube
A parametrization of SASI is introduced that allows IceCube to identify the instability epoch and reconstruct its frequency, peak time, amplitude, and duration from Galactic supernova neutrino signals at sub-percent to ten-percent precision.