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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Fast flavor conversion of neutrinos bifurcates supernova explosion outcomes: it aids shock revival in low-mass progenitors but inhibits it in higher-mass ones, controlled by mass accretion rate.
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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Bifurcated Impact of Neutrino Fast Flavor Conversion on Core-collapse Supernovae Informed by Multi-angle Neutrino Radiation Hydrodynamics
Fast flavor conversion of neutrinos bifurcates supernova explosion outcomes: it aids shock revival in low-mass progenitors but inhibits it in higher-mass ones, controlled by mass accretion rate.
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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.