Pairing instabilities in neutrino plasmas arise only with occupation number discontinuities and are spurious artifacts of energy discretization that disappear in the continuum.
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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.
A WKB ray-tracing framework shows that supernova matter gradients sweep flavomons through the unstable wavenumber range, strongly limiting slow-instability growth below the shock while leaving growth outside it largely intact.
In post-merger disks, electron-lepton-number crossings drive fast flavor instabilities that enhance heavy lepton neutrino fluxes, while collisional instabilities are subdominant and asymmetrically raise heavy-flavor antineutrino energies.
citing papers explorer
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Neutrino-antineutrino superfluidity
Pairing instabilities in neutrino plasmas arise only with occupation number discontinuities and are spurious artifacts of energy discretization that disappear in the continuum.
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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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Flavomons in Matter Gradients: Ray Tracing and Amplitude Evolution
A WKB ray-tracing framework shows that supernova matter gradients sweep flavomons through the unstable wavenumber range, strongly limiting slow-instability growth below the shock while leaving growth outside it largely intact.
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Neutrino transport and flavor instabilities in a post-merger disk
In post-merger disks, electron-lepton-number crossings drive fast flavor instabilities that enhance heavy lepton neutrino fluxes, while collisional instabilities are subdominant and asymmetrically raise heavy-flavor antineutrino energies.