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

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

1996-02-16

arxiv.org/abs/hep-ph/9602333v1

Phys.Rev.D54:7057-7066,1996

Physics

High Energy Physics

High Energy Physics - Phenomenology

23 pages, revtex; texfile and figures available also as one tar-compressed, uuencoded file from ftp://ftp.sns.ias.edu/pub/kras

Scientific paper

10.1103/PhysRevD.54.7057

We study the stability of the two--neutrino MSW solution of the solar neutrino problem, corresponding to solar $\nu_e$ transitions into sterile neutrino, $\nu_e \rightarrow \nu_s$, with respect to changes of the total fluxes of $^{8}$B and $^{7}$Be neutrinos, $\Phi_{{\rm B}}$ and $\Phi_{{\rm Be}}$. For any value of $\Phi_{{\rm Be}}$ from the interval $0.7\Phi^{{\rm BP}}_{{\rm Be}}\leq \Phi_{{\rm Be}} \leq 1.3\Phi^{{\rm BP}}_{{\rm Be}}$ (for $\Phi_{{\rm Be}} = 0.7\Phi^{{\rm BP}}_{{\rm Be}}$) the $\nu_e \rightarrow \nu_{s}$ MSW transitions provide at 95\% C.L. a description of the existing solar neutrino data for $0.40~(0.39)~\Phi^{{\rm BP}}_{{\rm B}} \ltap \Phi_{{\rm B}} \ltap 36~(40)\Phi^{{\rm BP}}_{{\rm B}}$, $\Phi^{{\rm BP}}_{{\rm B}}$ and $\Phi^{{\rm BP}}_{{\rm Be}}$ 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 $\nu_e \rightarrow \nu_s$ solutions for the future solar neutrino experiments are considered as well.

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