The Dark Side of the Solar Neutrino Parameter Space

Results of neutrino oscillation experiments have always been presented on the(sin^2 2theta, Delta m^2) parameter space for the case of two-flavoroscillations. We point out, however, that this parameterization misses the halfof the parameter space pi/4 < theta <= pi/2 (``the dark side'...

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Detalles Bibliográficos
Autores principales: de Gouvea, Andre, Friedland, Alexander, Murayama, Hitoshi
Lenguaje:eng
Publicado: 2000
Materias:
Particle Physics - Phenomenology
Acceso en línea:https://dx.doi.org/10.1016/S0370-2693(00)00989-8
http://cds.cern.ch/record/425930
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author de Gouvea, Andre
Friedland, Alexander
Murayama, Hitoshi
author_facet de Gouvea, Andre
Friedland, Alexander
Murayama, Hitoshi
author_sort de Gouvea, Andre
collection CERN
description Results of neutrino oscillation experiments have always been presented on the(sin^2 2theta, Delta m^2) parameter space for the case of two-flavoroscillations. We point out, however, that this parameterization misses the halfof the parameter space pi/4 < theta <= pi/2 (``the dark side''), which isphysically inequivalent to the region 0 <= theta <= pi/4 (``the light side'')in the presence of matter effects. The MSW solutions to the solar neutrinoproblem can extend to the dark side, especially if we take the conservativeattitude to allow higher confidence levels, ignore some of the experimentalresults in the fits, or relax theoretical predictions. Furthermore even theso-called ``vacuum oscillation'' solution distinguishes the dark and the lightsides. We urge experimental collaborations to present their results on theentire parameter space.
id cern-425930
institution Organización Europea para la Investigación Nuclear
language eng
publishDate 2000
record_format invenio
spelling cern-4259302023-03-14T20:21:17Zdoi:10.1016/S0370-2693(00)00989-8http://cds.cern.ch/record/425930engde Gouvea, AndreFriedland, AlexanderMurayama, HitoshiThe Dark Side of the Solar Neutrino Parameter SpaceParticle Physics - PhenomenologyResults of neutrino oscillation experiments have always been presented on the(sin^2 2theta, Delta m^2) parameter space for the case of two-flavoroscillations. We point out, however, that this parameterization misses the halfof the parameter space pi/4 < theta <= pi/2 (``the dark side''), which isphysically inequivalent to the region 0 <= theta <= pi/4 (``the light side'')in the presence of matter effects. The MSW solutions to the solar neutrinoproblem can extend to the dark side, especially if we take the conservativeattitude to allow higher confidence levels, ignore some of the experimentalresults in the fits, or relax theoretical predictions. Furthermore even theso-called ``vacuum oscillation'' solution distinguishes the dark and the lightsides. We urge experimental collaborations to present their results on theentire parameter space.Results of neutrino oscillation experiments have always been presented on the (sin^2 2theta, Delta m^2) parameter space for the case of two-flavor oscillations. We point out, however, that this parameterization misses the half of the parameter space pi/4 < theta <= pi/2 (``the dark side''), which is physically inequivalent to the region 0 <= theta <= pi/4 (``the light side'') in the presence of matter effects. The MSW solutions to the solar neutrino problem can extend to the dark side, especially if we take the conservative attitude to allow higher confidence levels, ignore some of the experimental results in the fits, or relax theoretical predictions. Furthermore even the so-called ``vacuum oscillation'' solution distinguishes the dark and the light sides. We urge experimental collaborations to present their results on the entire parameter space.Results of neutrino oscillation experiments have always been presented on the (sin^2 2theta, Delta m^2) parameter space for the case of two-flavor oscillations. We point out, however, that this parameterization misses the half of the parameter space pi/4 < theta <= pi/2 (``the dark side''), which is physically inequivalent to the region 0 <= theta <= pi/4 (``the light side'') in the presence of matter effects. The MSW solutions to the solar neutrino problem can extend to the dark side, especially if we take the conservative attitude to allow higher confidence levels, ignore some of the experimental results in the fits, or relax theoretical predictions. Furthermore even the so-called ``vacuum oscillation'' solution distinguishes the dark and the light sides. We urge experimental collaborations to present their results on the entire parameter space.Results of neutrino oscillation experiments have always been presented on the (sin 2 2 θ , Δm 2 ) parameter space for the case of two-flavor oscillations. We point out, however, that this parameterization misses the half of the parameter space π 4 <θ≤ π 2 (`the dark side'), which is physically inequivalent to the region 0≤θ≤ π 4 (`the light side') in the presence of matter effects. The MSW solutions to the solar neutrino problem can extend to the dark side, especially if we take the conservative attitude to allow higher confidence levels, ignore some of the experimental results in the fits, or relax theoretical predictions. Furthermore, even the so-called `vacuum oscillation' solution distinguishes the dark and the light sides. We urge experimental collaborations to present their results on the entire parameter space.hep-ph/0002064UCB-PTH-00-03LBNL-45023LBL-45023CERN-TH-2000-043UCB-PTH-2000-03LBNL-45023oai:cds.cern.ch:4259302000-02-07
spellingShingle Particle Physics - Phenomenology
de Gouvea, Andre
Friedland, Alexander
Murayama, Hitoshi
The Dark Side of the Solar Neutrino Parameter Space
title The Dark Side of the Solar Neutrino Parameter Space
title_full The Dark Side of the Solar Neutrino Parameter Space
title_fullStr The Dark Side of the Solar Neutrino Parameter Space
title_full_unstemmed The Dark Side of the Solar Neutrino Parameter Space
title_short The Dark Side of the Solar Neutrino Parameter Space
title_sort dark side of the solar neutrino parameter space
topic Particle Physics - Phenomenology
url https://dx.doi.org/10.1016/S0370-2693(00)00989-8
http://cds.cern.ch/record/425930
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