On the MSW $ν_e \to ν_s$ transition solution of the solar neutrino problem

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dc.creatorKrastev, P. I.
dc.creatorPetcov, S. T.
dc.creatorQiuyu, L.
dc.date1996-02-16
dc.date.accessioned2026-07-07T10:33:17Z
dc.date.available2026-07-07T10:33:17Z
dc.descriptionWe study the stability of the two--neutrino MSW solution of the solar neutrino problem, corresponding to solar $ν_e$ transitions into sterile neutrino, $ν_e \rightarrow ν_s$, with respect to changes of the total fluxes of $^{8}$B and $^{7}$Be neutrinos, $Φ_{\rm B}$ and $Φ_{\rm Be}$. For any value of $Φ_{\rm Be}$ from the interval $0.7Φ^{\rm BP}_{\rm Be}\leq Φ_{\rm Be} \leq 1.3Φ^{\rm BP}_{\rm Be}$ (for $Φ_{\rm Be} = 0.7Φ^{\rm BP}_{\rm Be}$) the $ν_e \rightarrow ν_{s}$ MSW transitions provide at 95\% C.L. a description of the existing solar neutrino data for $0.40~(0.39)~Φ^{\rm BP}_{\rm B} \ltap Φ_{\rm B} \ltap 36~(40)Φ^{\rm BP}_{\rm B}$, $Φ^{\rm BP}_{\rm B}$ and $Φ^{\rm BP}_{\rm Be}$ being the fluxes in the solar model of Bahcall--Pinsonneault from 1992. The corresponding allowed regions of values of the parameters \dm2 and \sn2, characterizing the solar neutrino transitions, are derived. The physical implications of the found MSW $ν_e \rightarrow ν_s$ solutions for the future solar neutrino experiments are considered as well.
dc.description23 pages, revtex; texfile and figures available also as one tar-compressed, uuencoded file from ftp://ftp.sns.ias.edu/pub/krastev/STER (first three figures, when unpacked, are 6.9 Mb each !!!)
dc.identifierhttps://arxiv.org/abs/hep-ph/9602333
dc.identifierhttp://arxiv.org/abs/hep-ph/9602333
dc.identifierPhys.Rev.D54:7057-7066,1996
dc.identifierdoi:10.1103/PhysRevD.54.7057
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/179057
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectAstrophysics
dc.titleOn the MSW $ν_e \to ν_s$ transition solution of the solar neutrino problem
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