MSW effect and (anti) neutrinos from Sn1987A

Lagage, Pierre-Olivier; Cribier, M.; Rich, J.; Vignaud, D.

doi:10.1016/0370-2693(87)90469-2

Cited by 27 publications

(9 citation statements)

References 16 publications

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“…For the core crossing trajectories the effects can be enhanced due to parametric effects. 7). The identification of the Earth matter effect is possible in a single detector (in the LMA case) by the observation of the oscillatory modulation of the energy spectrum in the high energy part: E > 40 MeV.…”

Section: Discussionmentioning

confidence: 99%

“…The possibility exists that U e3 will be determined by MINOS [52] provided that its value is not too far from the present upper bound, eq. (7). In this case, U e3 is certainly in the adiabatic range.…”

mentioning

confidence: 84%

“…We use the density profile (4); the error in P H due to the uncertainty in the density profile is estimated to be within a factor of 2 [14]. The figure shows that as |U e3 | 2 decreases in the range allowed by the bound (7) the transition in the H resonance varies from perfectly adiabatic (P H ≃ 0), for |U e3 | 2 > ∼ 5 · 10 −4 , to strongly non-adiabatic (P H ≃ 1), for |U e3 | 2 < ∼ 10 −6 . The intervals of adiabaticity and strong adiabaticity violation change only mildly as ∆m 2 atm varies in the presently allowed range.…”

Section: Neutrino Channelsmentioning

confidence: 99%

“…In this region one expects the disappearance of the ν e flux due to conversion ν e → ν µ , ν τ inside the star. It was marked however that oscillations inside the Earth can regenerate the ν e flux, so that the bound is absent in the region of the large mixing angle (LMA) solution of the solar neutrino problem [5,6] (see also the discussions in [7,8]). In this context, it was shown that the existence of the Earth matter effect depends on the conversion in the high density resonance associated with the large ∆m 2 which is responsible for the oscillations of atmospheric neutrinos [9,10,11].…”

Section: Introductionmentioning

confidence: 99%

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Supernova neutrinos: Earth matter effects and neutrino mass spectrum

2001

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We perform a detailed study of the Earth matter effects on supernova neutrinos. The dependences of these effects on the properties of the original neutrino fluxes, on the trajectory of the neutrinos inside the Earth and on the oscillation parameters are described. We show that, for a large fraction (60 %) of the possible arrival times of the signal, the neutrino flux crosses a substantial amount of the matter of the Earth at least for one of the existing detectors. For oscillation parameters from the LMA solution of the solar neutrino problem the Earth matter effect consists in an oscillatory modulation of the $\barnue$ and/or $\nu_e$ energy spectra. The relative deviation with respect to the undistorted spectra can be as large as 20-30 % for E> 20 MeV and 70-100 % for E> 40 MeV. For parameters from the SMA and LOW solutions the effect is localized at low energies (E<10 MeV) and is not larger than 10 %. The Earth matter effects can be revealed (i) by the observation of oscillatory distortions of the energy spectra in a single experiment and (ii) by the comparison between the spectra at different detectors. For a supernova at distance D=10 Kpc, comparing the results of SuperKamiokande (SK), SNO and LVD experiments one can establish the effect at (2-3) \sigma level, whereas larger statistical significance ((4-5) \sigma) is obtained if two experiments of SK-size or larger are available. Studies of the Earth matter effect will select or confirm the solution of the solar neutrino problem, probe the mixing U_{e 3} and identify the hierarchy of the neutrino mass spectrum.Comment: LaTeX, 54 pages, 21 figures. Slight modifications in the discussion on the identification of Earth effects, minor changes in the figures and in the notation, typos corrected, references adde

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Section: Discussionmentioning

confidence: 99%

mentioning

confidence: 84%

Section: Neutrino Channelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Supernova neutrinos: Earth matter effects and neutrino mass spectrum

2001

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“…In fact, the events observed by IMB [16,17], Kamiokande-II [18,19] and Baksan [20], represent a historic opportunity to investigate the physics of the collapse and of the explosion. A very extensive literature testifies the effort to extract information from these data with a wide variety of methods [21,22,23,24,25,26,27,28,29,30,31,32,33,34,35,36,37,38,39,40,41,42,43,44]. Usually, a specific characteristic of the SN1987A data is studied, most frequently the energy distribution.…”

Section: Introductionmentioning

confidence: 99%

Improved analysis of SN1987A antineutrino events

Pagliaroli

Vissani

Costantini

et al. 2009

Astroparticle Physics

118

173

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We propose a new parameterization of the antineutrino flux from core collapse supernovae, that allows an interpretation of its astrophysical parameters within the Bethe and Wilson scenario for the explosion, and that leads to a reasonable (smooth) behavior of the average energy and of the luminosity curve. We apply it to analyze the events observed by Kamiokande-II, IMB and Baksan detectors in correlation with SN1987A. For the first time, we consider in the same analysis all data characteristics: times, energies and angles of the observed events. We account for the presence of background and evaluate the impact of neutrino oscillations. The hypothesis that the initial luminous phase of emission (accretion) is absent can be rejected at the 2 % significance level. Without the need to impose external priors in the likelihood analysis, the best-fit values of the astrophysical parameters are found to be in remarkable agreement with the expectations of the standard core-collapse scenario; in particular, the electron antineutrino-sphere radius is 16 km, the duration of the accretion phase is found to be 0.55 s, and the initial accreting mass is 0.22 M(sun). Similarly the total energy emitted in neutrinos is 2.2*10^{53} erg, again close to the expectations. The errors on the parameters are evaluated and found to be relatively large, consistently with the limited number of detected events; the two dimensional confidence regions, that demonstrate the main correlations between the parameters, are also given.Comment: 15 pages, 5 figure

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Massive Neutrinos

Langacker

1988

Neutrino Physics

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MSW effect and (anti) neutrinos from Sn1987A

Cited by 27 publications

References 16 publications

Supernova neutrinos: Earth matter effects and neutrino mass spectrum

Supernova neutrinos: Earth matter effects and neutrino mass spectrum

Improved analysis of SN1987A antineutrino events

Massive Neutrinos

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