Symmetries in collective neutrino oscillations

Duan, Huaiyu; Fuller, George M.; Qian, Yongzhong

doi:10.1088/0954-3899/36/10/105003

Cited by 52 publications

(88 citation statements)

References 52 publications

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“…This is consistent with the conclusions of [18] as S ⊥ does at the critical point in the single-angle approximation (see Fig. 4).…”

Section: Collective Neutrino Oscillations In Supernovaesupporting

confidence: 91%

Resonances driven by a neutrino gyroscope and collective neutrino oscillations in supernovae

Qian²

2011

Phys. Rev. D

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We show that flavor evolution of a system of neutrinos with continuous energy spectra as in supernovae can be understood in terms of the response of individual neutrino flavor-isospins (NFIS's) to the mean field. In the case of a system initially consisting of ν e andν e with the same energy spectrum but different number densities, the mean field is very well approximated by the total angular momentum of a neutrino gyroscope. Assuming that NFIS evolution is independent of the initial neutrino emission angle, the so-called single-angle approximation, we find that the evolution is governed by two types of resonances driven by precession and nutation of the gyroscope, respectively. The net flavor transformation crucially depends on the adiabaticity of evolution through these resonances. We show that the results for the system of two initial neutrino species can be extended to a system of four species with the initial number densities of ν e andν e significantly larger than those of ν x andν x . Further, we find that when the dependence on the initial neutrino emission angle is taken into account in the multi-angle approximation, nutation of the mean field is quickly damped out and can be neglected. In contrast, precession-driven resonances still govern the evolution of NFIS's with different energy and emission angles just as in the single-angle approximation. Our pedagogical and analytic study of collective neutrino oscillations in supernovae provides some insights into these seemingly complicated yet fascinating phenomena.

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“…This is consistent with the conclusions of [18] as S ⊥ does at the critical point in the single-angle approximation (see Fig. 4).…”

Section: Collective Neutrino Oscillations In Supernovaesupporting

confidence: 91%

Resonances driven by a neutrino gyroscope and collective neutrino oscillations in supernovae

Qian²

2011

Phys. Rev. D

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“…Nutation oscillations are a high neutrino density phenomenon that have been deeply studied in the supernova setting, e.g. [30]. They have also been studied in the disk setting, [17,18].…”

Section: A Single Disk Modelsmentioning

confidence: 99%

“…At very high densities of neutrinos, more than one type of synchronized neutrino oscillation can occur, e.g. [28][29][30]. At very low densities of neutrinos, the neutrino self interaction potential is unimportant and Mikheyev Smirnov Wolfenstein (MSW) oscillations can take place when the scale of the matter potential is the same as the vacuum scale.…”

Section: Introductionmentioning

confidence: 99%

Symmetric and standard matter neutrino resonances above merging compact objects

2016

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Matter-neutrino resonances (MNR) can occur in environments where the flux of electron antineutrinos is greater than the flux of electron neutrinos. These resonances may result in dramatic neutrino flavor transformation. Compact object merger disks are an example of an environment where electron antineutrinos outnumber neutrinos. We study MNR resonances in several such disk configurations and find two qualitatively different types of matter-neutrino resonances: a standard MNR and a symmetric MNR. We examine the transformation that occurs in each type of resonance and explore the consequences for nucleosynthesis.

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“…The self-interaction term from neutrino-neutrino scattering generates nonlinear effects that only recently have been studied in detail in the context of supernovae [7,25,34,40,41,42,43,44,45,46,47,48,49]. The character of the neutrino conversion is roughly determined by the relative size of the different frequencies ω ji , ω e , and ω ν .…”

Section: Flavor Conversion In the Star And In The Earth: Generalmentioning

confidence: 99%

Neutrino oscillation signatures of oxygen-neon-magnesium supernovae

2008

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We discuss the flavor conversion of neutrinos from core collapse supernovae that have oxygenneon-magnesium (ONeMg) cores. Using the numerically calculated evolution of the star up to 650 ms post bounce, we find that, for the normal mass hierarchy, the electron neutrino flux in a detector shows signatures of two typical features of an ONeMg-core supernova: a sharp step in the density profile at the base of the He shell and a faster shock wave propagation compared to iron core supernovae. Before the shock hits the density step (t < ∼ 150 ms), the survival probability of electron neutrinos above ∼20 MeV of energy is about ∼ 0.68, in contrast to values of ∼ 0.32 or less for an iron core supernova. The passage of the shock through the step and its subsequent propagation cause a decrease of the survival probability and a decrease of the amplitude of oscillations in the Earth, reflecting the transition to a more adiabatic propagation inside the star. These changes affect the lower energy neutrinos first; they are faster and more sizable for larger θ13. They are unique of ONeMg-core supernovae, and give the possibility to test the speed of the shock wave. The time modulation of the Earth effect and its negative sign at the neutronization peak are the most robust signatures in a detector.

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Symmetries in collective neutrino oscillations

Cited by 52 publications

References 52 publications

Resonances driven by a neutrino gyroscope and collective neutrino oscillations in supernovae

Resonances driven by a neutrino gyroscope and collective neutrino oscillations in supernovae

Symmetric and standard matter neutrino resonances above merging compact objects

Neutrino oscillation signatures of oxygen-neon-magnesium supernovae

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