Neutrino–neutrino interactions and flavour mixing in dense matter

Balantekin, A. B.; Pehlivan, Y.

doi:10.1088/0954-3899/34/1/004

Cited by 128 publications

(131 citation statements)

References 28 publications

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“…Perturbations of the (cylindrically symmetric) bulb model for neutrino emission might also be considered in more advanced simulations. Finally, there is a continuing interest in more formal aspects of the mean-field approach to neutrino self-interaction effects [61], which has been implicitly assumed in most of the related literature (including this work); see [62] for a recent discussion of its validity and inherent approximations.…”

Section: Conclusion and Prospectsmentioning

confidence: 99%

Collective neutrino flavor transitions in supernovae and the role of trajectory averaging

Fogli

Lisi

Marrone

et al. 2007

J. Cosmol. Astropart. Phys.

274

397

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Abstract. Non-linear effects on supernova neutrino oscillations, associated with neutrino-neutrino interactions, are known to induce collective flavor transformations near the supernova core for θ 13 = 0. In scenarios with very shallow electron density profiles, these transformations have been shown to couple with ordinary matter effects, jointly producing spectral distortions both in normal and inverted hierarchy. In this work we consider a complementary scenario, characterized by higher electron density, as indicated by shock-wave simulations during a few seconds after bounce. In this case, early collective flavor transitions are decoupled from later, ordinary matter effects. Moreover, such transitions become more amenable to both numerical computations and analytical interpretations in inverted hierarchy, while they basically vanish in normal hierarchy. We numerically evolve the neutrino density matrix in the region relevant for self-interaction effects, using thermal spectra and a representative value sin 2 θ 13 = 10 −4 . In the approximation of averaged intersection angle between neutrino trajectories, our simulations neatly show the collective phenomena of synchronization, bipolar oscillations, and spectral split, with analytically understandable features, as recently discussed in the literature. In the more realistic (but computationally demanding) case of non-averaged neutrino trajectories, our simulations do not show new significant qualitative features, apart from the smearing of "fine structures" such as bipolar nutations. Our results seem to suggest that, at least for non-shallow matter density profiles, averaging over neutrino trajectories plays a minor role in the final outcome. In this case, the swap of ν e and ν µ,τ spectra above a critical energy may represent an unmistakable signature of the inverted neutrino hierarchy, especially for θ 13 small enough to render further (ordinary or even turbulent) matter effects irrelevant.PACS numbers: 14.60. Pq, 13.15.+g, 97.60.Bw Collective neutrino flavor transitions in supernovae and the role of trajectory averaging 2

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Section: Conclusion and Prospectsmentioning

confidence: 99%

Collective neutrino flavor transitions in supernovae and the role of trajectory averaging

Fogli

Lisi

Marrone

et al. 2007

J. Cosmol. Astropart. Phys.

274

397

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“…The neutrinos streaming from a supernova (SN) core or from the accretion torus of coalescing neutron stars are so dense that the neutrino-neutrino interaction causes collective flavor transformations [1,2,3,4,5,6,7,8,9,10,11,12,13,14,15,16,17,18,19,20,21,22,23,24,25,26,27,28]. At the same time, the density of ordinary matter is also very large, suppressing normal flavor conversions unless the neutrinos encounter an MSW resonance [29,30,31,32].…”

Section: Introductionmentioning

confidence: 99%

Role of dense matter in collective supernova neutrino transformations

et al. 2008

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For neutrinos streaming from a supernova (SN) core, dense matter suppresses self-induced flavor transformations if the electron density ne significantly exceeds the neutrino density nν in the conversion region. If ne is comparable to nν one finds multi-angle decoherence, whereas the standard self-induced transformation behavior requires that in the transformation region nν is safely above ne. This condition need not be satisfied in the early phase after SN core bounce. Our new multi-angle effect is a subtle consequence of neutrinos traveling on different trajectories when streaming from a source that is not point-like.

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“…Introducing the creation and annihilation operators for one neutrino with three momentum p, we can write down the generators of an SU(2) algebra [48]:…”

Section: Neutrino Many-body Theorymentioning

confidence: 99%

Symmetries, Supersymmetries, and Pairing in Nuclei

Balantekin¹,

Bijker²,

Castaños³

et al. 2011

AIP Conference Proceedings

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These summer school lectures cover the use of algebraic techniques in various subfields of nuclear physics. After a brief description of groups and algebras, concepts of dynamical symmetry, dynamical supersymmetry, and supersymmetric quantum mechanics are introduced. Appropriate tools such as quasiparticles, quasispin, and Bogoliubov transformations are discussed with an emphasis on group theoretical foundations of these tools. To illustrate these concepts three physics applications are worked out in some detail: i) Pairing in nuclear physics; ii) Subbarrier fusion and associated group transformations; and iii) Symmetries of neutrino mass and of a related neutrino many-body problem.

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Neutrino–neutrino interactions and flavour mixing in dense matter

Cited by 128 publications

References 28 publications

Collective neutrino flavor transitions in supernovae and the role of trajectory averaging

Collective neutrino flavor transitions in supernovae and the role of trajectory averaging

Role of dense matter in collective supernova neutrino transformations

Symmetries, Supersymmetries, and Pairing in Nuclei

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