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Collective Neutrino Flavor Transformation In Supernovae
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abstract
We examine coherent active-active channel neutrino flavor evolution in environments where neutrino-neutrino forward scattering can engender large-scale collective flavor transformation. We point out a key quantity, the "total effective energy", which is conserved in several important regimes. Using this concept, we analyze collective neutrino and antineutrino flavor oscillation in the "synchronized" mode and what we term the "bi-polar" mode. We thereby are able to explain why large collective flavor mixing can develop on short timescales even when vacuum mixing angles are small in, e.g., a dense gas of initially pure $\nu_e$ and $\bar\nu_e$ with an inverted neutrino mass hierarchy (an example of bi-polar oscillation). In the context of the spin precession analogy, we find that the co-rotating frame provides insights into more general systems, where either the synchronized or bi-polar modes could arise. For example, we use the co-rotating frame to demonstrate how large flavor mixing in the bi-polar mode can occur in the presence of a large and dominant matter background. We use the adiabatic condition to derive a simple criterion for determining whether the synchronized or bi-polar mode will occur. Based on this criterion we predict that neutrinos and antineutrinos emitted from a proto-neutron star in a core-collapse supernova event can experience synchronized and bi-polar flavor transformations in sequence before conventional Mikhyev-Smirnov-Wolfenstein (MSW) flavor evolution takes over. This certainly will affect the analyses of future supernova neutrino signals, and might affect the treatment of shock re-heating rates and nucleosynthesis depending on the depth at which collective transformation arises.
Forward citations
Cited by 12 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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Advection Algorithms for Quantum Neutrino Moment Transport
A modulus-phase Riemann solver for quantum neutrino moments gives fast-flavor instability growth rates and wavenumbers closer to multi-angle simulations than the prior real-imaginary implementation.
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Solar-System Abundances of $p$-Nuclides Probe Collective Neutrino Oscillations in Supernovae
Nearby neutrino flavor conversion in a supernova can boost νp-process yields of p-nuclides like 92Mo and 92Nb by up to two orders of magnitude, matching solar abundances when conversion starts within ~10 km of the pro...
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Single-wave solutions of the neutrino fast flavor system. Part I. Mechanical properties
Single-wave neutrino flavor solutions form a non-integrable spin system without Gaudin invariants, so an exact flavor pendulum exists only for two beams and does not extend to continuous angle distributions.
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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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Comparative Testing of Subgrid Models for Fast Neutrino Flavor Conversions in Core-collapse Supernova Simulations
A 1D supernova simulation with four-species BGK subgrid modeling shows that three-species assumptions overestimate flavor conversion and that semi-implicit time integration is the most reliable.
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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 oscillations in a neutrino-dominated accretion disk around a Kerr BH
Neutrino self-interactions inside neutrino-cooled accretion disks are argued to push flavors toward equipartition, reducing the neutrino-antineutrino annihilation energy deposition around black holes by a factor up to...
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Impact of Neutrino Flavour Conversion on the Diffuse Neutrino Background from Neutrino-dominated Accretion Flows
Neutrino flavour conversion strongly suppresses the diffuse neutrino background from neutrino-dominated accretion flows if the neutrino mass ordering is inverted, leaving a detectable signal only in the normal ordering.
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Neutrino mass ordering from the next Galactic supernova at DUNE, HK, and JUNO
Neutronization burst and accretion-phase rise-time observables from a 10 kpc core-collapse supernova enable DUNE, HK and JUNO to discriminate neutrino mass ordering at 3-6 sigma using multiple progenitor simulations.
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Singular Perturbations of Hamilton-Jacobi Equations in the Wasserstein Space
The abstract claims a singular-perturbation limit theorem for second-order Hamilton-Jacobi equations on the Wasserstein space, but the submitted full text does not contain that paper.
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