Majorana neutrinos convert to antineutrinos in ultralight vector dark matter backgrounds coupled to lepton number, enabling supernova neutrino detectors to probe gauge couplings as small as 10^{-32} for masses around 10^{-22} to 10^{-14} eV.
Exploiting a future galactic supernova to probe neutrino magnetic moments
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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.
In the minimal B-L gauge extension, Majorana neutrinos at high breaking scale produce flat GW spectra from cosmic strings, Dirac at low scale produce peaked spectra from first-order phase transitions, and pseudo-Dirac produce kink features from domain wall annihilation.
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Neutrino-Antineutrino Conversion from Ultralight Vector Dark Matter
Majorana neutrinos convert to antineutrinos in ultralight vector dark matter backgrounds coupled to lepton number, enabling supernova neutrino detectors to probe gauge couplings as small as 10^{-32} for masses around 10^{-22} to 10^{-14} eV.
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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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Gravitational Wave Signature and the Nature of Neutrino Masses: Majorana, Dirac, or Pseudo-Dirac?
In the minimal B-L gauge extension, Majorana neutrinos at high breaking scale produce flat GW spectra from cosmic strings, Dirac at low scale produce peaked spectra from first-order phase transitions, and pseudo-Dirac produce kink features from domain wall annihilation.