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Flavor instabilities in the neutrino line model
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A dense neutrino medium can experience collective flavor oscillations through nonlinear neutrino-neutrino refraction. To make this multi-dimensional flavor transport problem more tractable, all existing studies have assumed certain symmetries (e.g., the spatial homogeneity and directional isotropy in the early universe) to reduce the dimensionality of the problem. In this work we show that, if both the directional and spatial symmetries are not enforced in the neutrino line model, collective oscillations can develop in the physical regimes where the symmetry-preserving oscillation modes are stable. Our results suggest that collective neutrino oscillations in real astrophysical environments (such as core-collapse supernovae and black-hole accretion discs) can be qualitatively different from the predictions based on existing models in which spatial and directional symmetries are artificially imposed.
Forward citations
Cited by 4 Pith papers
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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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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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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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Neutrino halo effect on collective neutrino oscillation in iron core-collapse supernova model of a 9.6 $M_{\odot}$ star
For a 9.6 solar mass supernova, including scattered halo neutrinos delays the onset of collective neutrino oscillation at early times and sharpens spectral swap features, improving their detectability.
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