Probing supernova shock waves and neutrino flavour transitions in next-generation water Cherenkov detectors

Fogli, G. L.; Lisi, E.; Mirizzi, Alessandro; Montanino, D.

doi:10.1088/1475-7516/2005/04/002

Cited by 110 publications

(136 citation statements)

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“…The expected neutrino energies from core-collapse SNe are of practical importance for sensitivity forecasts of a future galactic SN neutrino detection, in particular with regard to neutrino mixing parameters [18][19][20][21][22][23][24][25][26][27]. The expected energies are also important in the context of current limits and future detection possibilities of the diffuse SN neutrino background from all SNe in the universe [33][34][35][36][37].…”

Section: Discussion and Summarymentioning

confidence: 99%

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Analysis of the SN 1987A neutrinos with a flexible spectral shape

Mirizzi

Raffelt

2005

Phys. Rev. D

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We analyze the neutrino events from the supernova (SN) 1987A detected by the Kamiokande II (KII) and Irvine-Michigan-Brookhaven (IMB) experiments. For the time-integrated flux we assume a quasi-thermal spectrum of the form (E/E0) α e −(α+1)E/E 0 where α plays the role of a spectral index. This simple representation not only allows one to fit the total energy Etot emitted inνe and the average energy Eν e , but also accommodates a wide range of shapes, notably anti-pinched spectra that are broader than a thermal distribution. We find that the pile-up of low-energy events near threshold in KII forces the best-fit value for α to the lowest value of any assumed prior range. This applies to the KII events alone as well as to a common analysis of the two data sets. The preference of the data for an "unphysical" spectral shape implies that one can extract meaningful values for Eν e and Etot only if one fixes a prior value for α. The tension between the KII and IMB data sets and theoretical expectations for Eν e is not resolved by an anti-pinched spectrum.PACS numbers: 14.60. Pq, 95.55.Vj, 95.85.Ry, 97.60.Bw

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Section: Discussion and Summarymentioning

confidence: 99%

“…Of course, the relatively subtle modifications caused by Earth matter effects can be crucial for identifying the neutrino mass ordering from the high-statistics neutrino signal of a future galactic SN [18][19][20][21][22][23][24][25][26][27].…”

Section: Introductionmentioning

confidence: 99%

Analysis of the SN 1987A neutrinos with a flexible spectral shape

Mirizzi

Raffelt

2005

Phys. Rev. D

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“…Shock waves propagating during the first few second after bounce can produce very interesting MSW effects when λ ∼ ω, provided that sin 2 θ 13 is not too small [4][5][6][7][8][9][10][11]. For the typical (time-dependent) matter profiles used in these studies, such effects usually emerge in the first ∼ 10 s after a few hundred kilometers from the SN core, in which case collective neutrino self-interaction effects are already completely developed, as we shall see later.…”

Section: Matter Profilementioning

confidence: 99%

“…Mikheev-Smirnov-Wolfenstein (MSW) effects induced on neutrinos by background matter [3] have been widely studied as a tool to probe both neutrino masses and mixings and the SN dynamics. Recent examples include the characterization, at the level of observable SN neutrino event spectra, of shock-wave evolution effects after bounce [4][5][6][7][8][9][10][11][12][13] and of it possible "erasing" by stochastic matter fluctuations induced by turbulence [14][15][16].…”

Section: Introductionmentioning

confidence: 99%

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

Fogli

Lisi

Marrone

et al. 2007

J. Cosmol. Astropart. Phys.

273

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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“…The DSN search of the SK experiment is currently performed in the energy range 13 E ν 90 MeV [2,3], in which the dominant interaction mechanism, sensitive tō ν e 's only, is inverse β decay of free protons in the water molecule [12],ν e + p → e + + n.…”

Section: Introductionmentioning

confidence: 99%

Estimate of the theoretical uncertainty of the cross sections for nucleon knockout in neutral-current neutrino-oxygen interactions

Ankowski¹,

Bárbaro²,

Benhar³

et al. 2015

Phys. Rev. C

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Free nucleons propagating in water are known to produce γ rays, which form a background to the searches for diffuse supernova neutrinos and sterile neutrinos carried out with Cherenkov detectors. As a consequence, the process of nucleon knockout induced by neutral-current quasielastic interactions of atmospheric (anti)neutrinos with oxygen needs to be under control at the quantitative level in the background simulations of the ongoing and future experiments. In this paper, we provide a quantitative assessment of the uncertainty associated with the theoretical description of the nuclear cross sections, estimating it from the discrepancies between the predictions of different models.

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Probing supernova shock waves and neutrino flavour transitions in next-generation water Cherenkov detectors

Cited by 110 publications

References 50 publications

Analysis of the SN 1987A neutrinos with a flexible spectral shape

Analysis of the SN 1987A neutrinos with a flexible spectral shape

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

Estimate of the theoretical uncertainty of the cross sections for nucleon knockout in neutral-current neutrino-oxygen interactions

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