Stringent constraints on cosmological neutrino-antineutrino asymmetries from synchronized flavor transformation

Abazajian, Kevork N.; Beacom, J. F.; Bell, Nicole F.

doi:10.1103/physrevd.66.013008

Cited by 214 publications

(250 citation statements)

References 57 publications

(36 reference statements)

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“…Because of neutrino-neutrino forward scattering or neutrino self-interaction [1,2,3] neutrinos can experience collective flavour transformation in environments such as the early Universe (e.g., [4,5,6,7,8,9]) and supernovae (e.g., [10,11,12,13]) where neutrino number densities can be very large. This phenomenon is different from the conventional Mikheyev-Smirnov-Wolfenstein (MSW) effect [14,15] in that the flavour evolution histories of neutrinos in collective oscillations are coupled together and must be solved simultaneously.…”

Section: Introductionmentioning

confidence: 99%

Symmetries in collective neutrino oscillations

Duan¹,

Fuller²,

Qian³

2009

J. Phys. G: Nucl. Part. Phys.

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Abstract. We discuss the relationship between a symmetry in the neutrino flavour evolution equations and neutrino flavour oscillations in the collective precession mode. This collective precession mode can give rise to spectral swaps (splits) when conditions can be approximated as homogeneous and isotropic. Multi-angle numerical simulations of supernova neutrino flavour transformation show that when this approximation breaks down, non-collective neutrino oscillation modes decohere kinematically, but the collective precession mode still is expected to stand out. We provide a criterion for significant flavour transformation to occur if neutrinos participate in a collective precession mode. This criterion can be used to understand the suppression of collective neutrino oscillations in anisotropic environments in the presence of a high matter density. This criterion is also useful in understanding the breakdown of the collective precession mode when neutrino densities are small.

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Section: Introductionmentioning

confidence: 99%

Symmetries in collective neutrino oscillations

Duan¹,

Fuller²,

Qian³

2009

J. Phys. G: Nucl. Part. Phys.

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“…The resulting equations in principle include the effects of collisions as well as the non-linearities arising from neutrino forward scattering off a neutrino background. They have been implemented to study the evolution of the neutrino distribution functions in the early Universe [6,27,28,29,30,31], in supernovae [32,33,34] as well as to study the relic neutrino asymmetry [35]. Novel fascinating self-synchronization phenomena emerges as a consequence of the non-linearities in a neutrino background with potential implications on CP (and baryon) asymmetry in the early Universe [6,28].…”

Section: Introductionmentioning

confidence: 99%

Oscillations and evolution of a hot and dense gas of flavor neutrinos: A quantum field theory study

Boyanovsky

2004

Phys. Rev. D

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We study the time evolution of the distribution functions for hot and or degenerate gases of two flavors of Dirac neutrinos as a result of flavor mixing and dephasing. This is achieved by obtaining the time evolution of the flavor density matrix directly from quantum field theory at finite temperature and density. The time evolution features a rich hierarchy of scales which are widely separated in the nearly degenerate or relativistic cases and originate in interference phenomena between particle and antiparticle states. In the degenerate case the flavor asymmetry ∆N (t) relaxes to the asymptotic limit ∆N (∞) = ∆N (0) cos 2 (2θ) via dephasing resulting from the oscillations between flavor modes that are not Pauli blocked, with a power law 1/t for t > ts ≈ 2kF /∆M 2 . kF is the largest of the Fermi momenta. The distribution function for flavor neutrinos and antineutrinos as well as off-diagonal densities are obtained. Flavor particle-antiparticle pairs are produced by mixing and oscillations with typical momentum k ∼M the average mass of the neutrinos. An effective field theory description emerges on long time scales in which the Heisenberg operators obey a Bloch-type equation of motion valid in the relativistic and nearly degenerate cases. We find the non-equilibrium propagators and correlation functions in this effective theory and discuss its regime of validity as well as the potential corrections.

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“…Neutrino propagation in dense matter [1,2] is encountered near the core of a core-collapse supernovae [3,4,5,6,7,8], in the Early Universe [9,10], and possibly in the gamma-ray bursts [11]. In particular, neutrino interactions play a crucial role in core-collapse supernovae.…”

Section: Introductionmentioning

confidence: 99%

Neutrino–neutrino interactions and flavour mixing in dense matter

Balantekin

Pehlivan

2006

J. Phys. G: Nucl. Part. Phys.

124

130

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An algebraic approach to the neutrino propagation in dense media is presented. The Hamiltonian describing a gas of neutrinos interacting with each other and with background fermions is written in terms of the appropriate SU(N) operators, where N is the number of neutrino flavors. The evolution of the resulting many-body problem is formulated as a coherent-state path integral. Some commonly used approximations are shown to represent the saddle-point solution of the path integral for the full many-body system.

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Stringent constraints on cosmological neutrino-antineutrino asymmetries from synchronized flavor transformation

Cited by 214 publications

References 57 publications

Symmetries in collective neutrino oscillations

Symmetries in collective neutrino oscillations

Oscillations and evolution of a hot and dense gas of flavor neutrinos: A quantum field theory study

Neutrino–neutrino interactions and flavour mixing in dense matter

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