Solar-neutrino oscillations and third-flavour admixture

With one \Delta m^2 of the appropriate order of magnitude to solve the atmospheric neutrino problem, we study the resulting three-generation vacuum-oscillation fit to the solar neutrino flux. An explanation of the atmospheric neutrino composition in terms of pure \nu_\mu \to \nu_\tau oscillations is...

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Detalles Bibliográficos
Autores principales: Osland, P., Vigdel, G.
Lenguaje:eng
Publicado: 1998
Materias:
Particle Physics - Phenomenology
Acceso en línea:https://dx.doi.org/10.1016/S0370-2693(98)00973-3
http://cds.cern.ch/record/356913
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author Osland, P.
Vigdel, G.
author_facet Osland, P.
Vigdel, G.
author_sort Osland, P.
collection CERN
description With one \Delta m^2 of the appropriate order of magnitude to solve the atmospheric neutrino problem, we study the resulting three-generation vacuum-oscillation fit to the solar neutrino flux. An explanation of the atmospheric neutrino composition in terms of pure \nu_\mu \to \nu_\tau oscillations is easily compatible with the well-known two-flavour oscillation solution for solar neutrinos. The allowed parameter region in the the mixing element U_{e3}, provided this is less than about 0.4. We find that the threefold maximal mixing is disfavoured.
id cern-356913
institution Organización Europea para la Investigación Nuclear
language eng
publishDate 1998
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spelling cern-3569132023-03-14T20:35:11Zdoi:10.1016/S0370-2693(98)00973-3http://cds.cern.ch/record/356913engOsland, P.Vigdel, G.Solar-neutrino oscillations and third-flavour admixtureParticle Physics - PhenomenologyWith one \Delta m^2 of the appropriate order of magnitude to solve the atmospheric neutrino problem, we study the resulting three-generation vacuum-oscillation fit to the solar neutrino flux. An explanation of the atmospheric neutrino composition in terms of pure \nu_\mu \to \nu_\tau oscillations is easily compatible with the well-known two-flavour oscillation solution for solar neutrinos. The allowed parameter region in the the mixing element U_{e3}, provided this is less than about 0.4. We find that the threefold maximal mixing is disfavoured.With one \Delta m^2 of the appropriate order of magnitude to solve the atmospheric neutrino problem, we study the resulting three-generation vacuum-oscillation fit to the solar neutrino flux. An explanation of the atmospheric neutrino composition in terms of pure \nu_\mu \to \nu_\tau oscillations is easily compatible with the well-known two-flavour oscillation solution for solar neutrinos. The allowed parameter region in the \sin^2(2\theta_{12})--\Delta m^2 plane changes little with increasing values of the mixing element U_{e3}, provided this is less than about 0.4. We find that the threefold maximal mixing is disfavoured.With one \Delta m^2 of the appropriate order of magnitude to solve the atmospheric neutrino problem, we study the resulting three-generation vacuum-oscillation fit to the solar neutrino flux. An explanation of the atmospheric neutrino composition in terms of pure \nu_\mu \to \nu_\tau oscillations is easily compatible with the well-known two-flavour oscillation solution for solar neutrinos. The allowed parameter region in the \sin^2(2\theta_{12})--\Delta m^2 plane changes little with increasing values of the mixing element U_{e3}, provided this is less than about 0.4. We find that the threefold maximal mixing is disfavoured.With one \Delta m^2 of the appropriate order of magnitude to solve the atmospheric neutrino problem, we study the resulting three-generation vacuum-oscillation fit to the solar neutrino flux. An explanation of the atmospheric neutrino composition in terms of pure \nu_\mu \to \nu_\tau oscillations is easily compatible with the well-known two-flavour oscillation solution for solar neutrinos. The allowed parameter region in the \sin^2(2\theta_{12})--\Delta m^2 plane changes little with increasing values of the mixing element U_{e3}, provided this is less than about 0.4. We find that the threefold maximal mixing is disfavoured.With one Δm 2 of the appropriate order of magnitude to solve the atmospheric neutrino problem, we study the resulting three-generation vacuum-oscillation fit to the solar neutrino flux. An explanation of the atmospheric neutrino composition in terms of pure ν μ → ν τ oscillations is easily compatible with the well-known two-flavour oscillation solution for solar neutrinos. The allowed parameter region in the sin 2 (2 θ 12 )– Δm 2 plane changes little with increasing values of the mixing element U e 3 , provided this is less than about 0.4. We find that the threefold maximal mixing is disfavoured.hep-ph/9806339CERN-TH-98-200CERN-TH-98-200oai:cds.cern.ch:3569131998-06-11
spellingShingle Particle Physics - Phenomenology
Osland, P.
Vigdel, G.
Solar-neutrino oscillations and third-flavour admixture
title Solar-neutrino oscillations and third-flavour admixture
title_full Solar-neutrino oscillations and third-flavour admixture
title_fullStr Solar-neutrino oscillations and third-flavour admixture
title_full_unstemmed Solar-neutrino oscillations and third-flavour admixture
title_short Solar-neutrino oscillations and third-flavour admixture
title_sort solar-neutrino oscillations and third-flavour admixture
topic Particle Physics - Phenomenology
url https://dx.doi.org/10.1016/S0370-2693(98)00973-3
http://cds.cern.ch/record/356913
work_keys_str_mv AT oslandp solarneutrinooscillationsandthirdflavouradmixture
AT vigdelg solarneutrinooscillationsandthirdflavouradmixture

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