Simulating nonlinear neutrino flavor evolution

Duan, Huaiyu; Fuller, George M.; Carlson, J.

doi:10.1088/1749-4699/1/1/015007

Cited by 49 publications

(75 citation statements)

References 83 publications

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“…We have also calculated the magnitude of flux |F x |, the magnitude of average velocity | v x | = |F x |/n x , and the effective neutrino-neutrino interaction strength µ x defined later in Eq. (31). We show contours of these quantities in Fig.…”

Section: Diskmentioning

confidence: 99%

“…Only recently has it been fully appreciated that this condition is sufficient even if a dense background of ordinary matter provides a much larger interaction energy so that naively neutrinoneutrino interactions would seem negligible [14,15]. Following this crucial insight, nonlinear oscillation phenomena in the supernova (SN) context have been studied over the past two years in a long series of papers [15,16,17,18,19,20,21,22,23,24,25,26,27,28,29,30,31].…”

Section: Introductionmentioning

confidence: 99%

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Collective neutrino oscillations in nonspherical geometry

et al. 2008

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The rich phenomenology of collective neutrino oscillations has been studied only in one-dimensional or spherically symmetric systems. Motivated by the non-spherical example of coalescing neutron stars, presumably the central engines of short gamma-ray bursts, we use the Liouville equation to formulate the problem for general source geometries. Assuming the neutrino ensemble displays self-maintained coherence, the problem once more becomes effectively one-dimensional along the streamlines of the overall neutrino flux. This approach for the first time provides a formal definition of the "single-angle approximation" frequently used for supernova neutrinos and allows for a natural generalization to non-spherical geometries. We study the explicit example of a diskshaped source as a proxy for coalescing neutron stars.

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Section: Diskmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Collective neutrino oscillations in nonspherical geometry

et al. 2008

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“…This epoch, before the delayed explosion finally takes off, is when the neutrino luminosity and the difference between theν e andν µ,τ fluxes are largest. If self-induced flavor conversion did not occur and the mixing angle θ 13 was not very small [20], the accretion phase would provide a plausible opportunity to determine the mass hierarchy [3,19].Numerical multi-angle simulations of collective oscillations are very demanding [21], but it is much easier to …”

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confidence: 99%

“…Numerical multi-angle simulations of collective oscillations are very demanding [21], but it is much easier to…”

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confidence: 99%

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Suppression of Self-Induced Flavor Conversion in the Supernova Accretion Phase

et al. 2012

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Self-induced flavor conversions of supernova (SN) neutrinos can strongly modify the flavor dependent fluxes. We perform a linearized flavor stability analysis with accretion-phase matter profiles of a 15 M spherically symmetric model and corresponding neutrino fluxes. We use realistic energy and angle distributions, the latter deviating strongly from quasi-isotropic emission, thus accounting for both multi-angle and multi-energy effects. For our matter and neutrino density profile we always find stable conditions: flavor conversions are limited to the usual Mikheyev-Smirnov-Wolfenstein effect. In this case one may distinguish the neutrino mass hierarchy in a SN neutrino signal if the mixing angle θ13 is as large as suggested by recent experiments.PACS numbers: 97.60.Bw, 14.60.PqIntroduction.-The huge neutrino fluxes emitted by core-collapse supernovae (SNe) are key to the explosion dynamics and nucleosynthesis [1] and detecting a highstatistics "neutrino light curve" from the next nearby SN is a major goal for neutrino astronomy [2]. Besides probing the core-collapse phenomenon in unprecedented detail, one may detect signatures of flavor oscillations and extract information on neutrino mixing parameters [3,4].The refractive effect caused by matter [5] suppresses flavor oscillations until neutrinos pass through the Mikheyev-Smirnov-Wolfenstein (MSW) region in the collapsing star's envelope [6,7]. However, neutrino-neutrino interactions, through a flavor off-diagonal refractive index [8,9], can trigger self-induced flavor conversions [10][11][12]. This collective effect usually occurs between the neutrino sphere and the MSW region and can strongly modify neutrino spectra [13][14][15], although this would never seem to help explode the star [16]. Actually, in lowmass SNe (not studied here) the density falls off so fast that MSW can occur first, leading to novel effects on the prompt ν e burst [17].Collective oscillations at first seemed unaffected by matter because its influence does not depend on neutrino energies [13]. However, depending on emission angle, neutrinos accrue different matter-induced flavordependent phases until they reach a given radius. This "multi-angle matter effect" can suppress self-induced flavor conversion [18]. Based on schematic flux spectra, this was numerically confirmed for accretion-phase SN models where the density near the core is large [19]. This epoch, before the delayed explosion finally takes off, is when the neutrino luminosity and the difference between theν e andν µ,τ fluxes are largest. If self-induced flavor conversion did not occur and the mixing angle θ 13 was not very small [20], the accretion phase would provide a plausible opportunity to determine the mass hierarchy [3,19].Numerical multi-angle simulations of collective oscillations are very demanding [21], but it is much easier to

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Probing non-standard neutrino interactions with supernova neutrinos at Hyper-K

Lei

Steinberg

Wells

2020

J. High Energ. Phys.

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Non-standard neutrino self interactions (NSSI) could be stronger than Fermi interactions. We investigate the ability to constrain these four-neutrino interactions by their effect on the flux of neutrinos originating from a galactic supernova. In the dense medium of a core collapse supernova, these new self interactions can have a significant impact on neutrino oscillations, leading to changes at the flavor evolution and spectra level. We use simulations of the neutrino flux from a 13 solar mass, core collapse supernova at 10 kpc away, and numerically propagate these neutrinos through the stellar medium taking into account vacuum/MSW oscillations, SM ν − ν scattering as well as ν − ν interactions that arise from NSSI. We pass the resulting neutrino flux to a simulation of the future Hyper-Kamiokande detector to see what constraints on NSSI parameters are possible when the next galactic supernova becomes visible. We find that these constraints depend strongly on the neutrino mass hierarchy and if the NSSI is flavor-violating or preserving. Sensitivity to NSSI in the normal hierarchy (NH) at Hyper-K is limited by the experiment's ability to efficiently detect ν e , but deviations from no NSSI could be seen if the NSSI is particularly strong. In the inverted hierarchy (IH) scenario, Hyper-K can significantly improve constraints on flavor-violating NSSI down to O(10 −1 )G F .

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Simulating nonlinear neutrino flavor evolution

Cited by 49 publications

References 83 publications

Collective neutrino oscillations in nonspherical geometry

Collective neutrino oscillations in nonspherical geometry

Suppression of Self-Induced Flavor Conversion in the Supernova Accretion Phase

Probing non-standard neutrino interactions with supernova neutrinos at Hyper-K

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