### Abstract

After recent results from solar neutrino experiments and KamLAND we can definitely say that neutrinos from SN1987A underwent flavor conversion, and the conversion effects must be taken into account in the analysis of the data. Assuming the normal mass hierarchy of neutrinos we calculate the permutation factors p for the Kamiokande-2, IMB and Baksan detectors. The conversion inside the star leads to p=0.28-0.32; the oscillations in the matter of the Earth give partial (and different for different detectors) regeneration of the original ν̄_{e} signal, reducing this factor down to 0.15-0.20 (at E=40 MeV). We study in details the influence of conversion on the observed signal depending on the parameters of the original neutrino spectra. For a given set of these parameters, the conversion could lead to an increase of the average energy of the observed events up to 50% and of the number of events by a factor of 2 at Kamiokande-2 and by a factor of 3-5 at IMB. Inversely, we find that neglecting the conversion effects can lead up to 50% error in the determination of the average energy of the original ν̄_{e} spectrum and about 50% error in the original luminosity. Comparing our calculations with experimental data we conclude that the Kamiokande-2 data alone do not favor strong conversion effect, which testifies for small difference of the original ν̄_{e} and ν̄_{μ} spectra. In contrast, the combined analysis of the Kamiokande and IMB results slightly favors strong conversion effects (that is, large difference of the original spectra). In comparison with the no-oscillation case, the latter requires lower average energy and higher luminosity of the original ν̄_{e} flux.

Original language | English (US) |
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Pages (from-to) | 703-720 |

Number of pages | 18 |

Journal | Astroparticle Physics |

Volume | 21 |

Issue number | 6 |

DOIs | |

State | Published - Sep 1 2004 |

Externally published | Yes |

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### ASJC Scopus subject areas

- Astronomy and Astrophysics

### Cite this

*Astroparticle Physics*,

*21*(6), 703-720. https://doi.org/10.1016/j.astropartphys.2004.05.005