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Collision-induced flavor instability in dense neutrino gases with energy-dependent scattering
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We investigate the collision-induced flavor instability in homogeneous, isotropic, dense neutrino gases in the two-flavor mixing scenario with energy-dependent scattering. We uncover a simple expression of the growth rate of this instability in terms of the flavor-decohering collision rates and the electron lepton number distribution of the neutrino. This growth rate is common to the neutrinos and antineutrinos of different energies, and is independent of the mass-splitting and vacuum mixing angle of the neutrino, the matter density, and the neutrino density, although the initial amplitude of the unstable oscillation mode can be suppressed by a large matter density. Our results suggest that neutrinos are likely to experience collision-induced flavor conversions deep inside a core-collapse supernova even when both the fast and slow collective flavor oscillations are suppressed.
Forward citations
Cited by 8 Pith papers
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Collective flavor conversions are interactions of neutrinos with quantized flavor waves
Neutrino fast flavor instabilities are equivalent to stimulated emission of flavomons, quantum flavor waves, whose kinetic equations reproduce the linear growth rate and extend naturally beyond it.
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Theory of neutrino slow flavor evolution. Part I. Homogeneous medium
Slow neutrino flavor instabilities split into a new resonant small-scale branch with growth rate ~omega_E/epsilon and the familiar non-resonant branch with the traditional scale 1/sqrt(omega_E mu).
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Predicting the outcome of collisional neutrino flavor conversion
Collisional neutrino flavor instabilities settle into a state at the edge of instability with nonzero flavor coherence, and explicit formulas predict this final state.
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Neutrino quantum kinetics for fast flavor conversion in a time-dependent environment
Fast flavor conversion in a time-varying supernova background proceeds through three episodes and broadly agrees with static two-step model results.
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Flavor Equilibration of Supernova Neutrinos: Exploring the Dynamics of Slow Modes
Slow flavor conversion drives supernova neutrinos to a coarse-grained flavor-equilibrated state within a few inverse vacuum frequencies, with survival probabilities set by the neutrino-antineutrino density ratio alone.
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Neutrino flavor instabilities in a binary neutron star merger remnant: Roles of a long-lived hypermassive neutron star
In a long-lived hypermassive neutron star merger remnant, fast flavor instabilities occur transiently and locally while collisional flavor instabilities persist widely in the disk for about one second.
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Theory of neutrino slow flavor evolution. Part II. Space-time evolution of linear instabilities
All weak fast and slow neutrino flavor instabilities are convective, so they grow spatially along neutrino directions rather than locally in time.
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Fast Flavor Pendulum: Instability Condition
The Nyquist criterion for homogeneous fast flavor instability is corrected to N = W - Ns/2, where W is the subluminal winding number and Ns counts real superluminal solutions.
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