In anisotropic neutrino gases, νν-bar pairing instabilities emerge when the excessive pair-occupation number distribution changes sign, producing pair conversions at growth rates comparable to fast flavor instabilities.
Neutrino cloud instabilities just above the neutrino sphere of a supernova
5 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The usual treatments of the neutrino flavor-evolution, beyond a surface above the last scattering, assume identical angular distributions at this distance for the different initial (unmixed) flavors, and for particles and antiparticles. Taking into account differences in these distributions that must be present, as a result of the species-dependent scattering cross-sections lower down in the star, leads to a new set of non-linear equations. These equations are unstable, even at the initial surface, with respect to perturbations that have both tiny mixing from neutrino oscillations and that break all-over spherical-symmetry. There could be important consequences for: 1) the dynamics of the explosion, 2) R-process-nucleosynthesis, and 3) some future observable neutrino pulse.
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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.
MSW resonances in collapsing supermassive stars swap neutrino flavors adiabatically in the normal hierarchy for neutrinos and inverted hierarchy for antineutrinos, altering the initial 5:1 electron-to-muon/tau flux ratio.
Neutrino flavor conversion in supernova cores can enhance or suppress explodability depending on the conversion location, independent of progenitor mass.
Simulations of 195 stellar progenitors indicate that neutrino flavor conversion alters explodability and remnant mass distributions, particularly for stars of 16-30 solar masses.
citing papers explorer
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Collective neutrino-antineutrino pair oscillations
In anisotropic neutrino gases, νν-bar pairing instabilities emerge when the excessive pair-occupation number distribution changes sign, producing pair conversions at growth rates comparable to fast flavor instabilities.
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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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Neutrino Flavor Transformation in Collapsing Supermassive Objects
MSW resonances in collapsing supermassive stars swap neutrino flavors adiabatically in the normal hierarchy for neutrinos and inverted hierarchy for antineutrinos, altering the initial 5:1 electron-to-muon/tau flux ratio.
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Flavor Conversion Enhances or Suppresses Supernova Explodability Independent of the Progenitor Mass
Neutrino flavor conversion in supernova cores can enhance or suppress explodability depending on the conversion location, independent of progenitor mass.
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Neutrino Flavor Conversion Shapes the Rate of Failed Core-collapse Supernovae
Simulations of 195 stellar progenitors indicate that neutrino flavor conversion alters explodability and remnant mass distributions, particularly for stars of 16-30 solar masses.