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Title: Vacuum oscillation solutions of the solar neutrino problem

Abstract

We study the stability of the two-neutrino vacuum oscillation solution of the solar neutrino problem with respect to changes of the total fluxes of {sup 8}B and {sup 7}Be neutrinos, {Phi}{sub B} and {Phi}{sub B}{sub e}. For any value of {Phi}{sub B}{sub e} from the interval 0.7{Phi}{sub B}{sub e}{sup B}{sup P}{le}{Phi}{sub B}{sub e}{le}1.3{Phi}{sub B}{sub e}{sup B}{sup P} the solar {nu}{sub {ital e}} oscillations into an active neutrino, {nu}{sub {ital e}}{leftrightarrow}{nu}{sub {mu}}{sub (}{sub {tau}}{sub )}, provide at 95{percent} C.L. a description of the existing solar neutrino data for {Phi}{sub B}{approx_equal}(0.35{endash}3.4){Phi}{sub B}{sup B}{sup P}, {Phi}{sub B}{sup B}{sup P} and {Phi}{sub B}{sub e}{sup B}{sup P} being the fluxes in the solar model of Bahcall and Pinsonneault from 1992. For {Phi}{sub B}{sub e}{approx_equal}(0.7-1.3){Phi}{sub B}{sub e}{sup B}{sup P} we find also at 95- C.L. two new [one new] {nu}{sub {ital e}}{leftrightarrow}{nu}{sub {mu}}{sub (}{sub {tau}}{sub )} [{nu}{sub {ital e}}{leftrightarrow}{nu}{sub {ital s}}] oscillation solutions: (i) for {Phi}{sub B}{approx_equal}(0.35-0.43){Phi}{sub B}{sup B}{sup P} at {Delta}{ital m}{sup 2}{approx_equal}(4.7-6.5){times}10{sup {minus}}{sup 1}{sup 2} eV{sup 2} [(4.8-6.4){times}10{sup {minus}}{sup 1}{sup 2} eV{sup 2}] and sin{sup 2}2{theta}{approx_gt}0.71[0.74], and (ii) for {Phi}{sub B}{approx_equal}(0.45{endash}0.65){Phi}{sub B}{sup B}{sup P} at {Delta}{ital m}{sup 2}{approx_equal}(3.2-4.0){times}10{sup {minus}}{sup 1}{sup 1} eV{sup 2} and sin{sup 2}2{theta}{approx_gt}0.59. The physical implications of the new solutions formore » the future solar neutrino experiments are discussed. The data rule out at 97%-98%[99] C.L. the possibility of a universal (neutrino energy independent) suppression of the different components of the solar neutrino flux, resulting from solar {nu}{sub {ital e}} oscillations or transitions into active (sterile) neutrino. {copyright} {ital 1996 The American Physical Society.}« less

Authors:
 [1];  [2]
  1. School for Natural Sciences, Institute for Advanced Study, Princeton, New Jersey 08540 (United States)
  2. Scuola Internazionale Superiore di Studi Avanzati and Istituto Nazionale di Fizica Nucleare, Sezione di Trieste, I-34013 Trieste (Italy)
Publication Date:
OSTI Identifier:
282786
Resource Type:
Journal Article
Journal Name:
Physical Review, D
Additional Journal Information:
Journal Volume: 53; Journal Issue: 3; Other Information: PBD: Feb 1996
Country of Publication:
United States
Language:
English
Subject:
66 PHYSICS; SOLAR NEUTRINOS; NEUTRINO OSCILLATION; STABILITY; VACUUM STATES

Citation Formats

Krastev, P I, and Petcov, S T. Vacuum oscillation solutions of the solar neutrino problem. United States: N. p., 1996. Web. doi:10.1103/PhysRevD.53.1665.
Krastev, P I, & Petcov, S T. Vacuum oscillation solutions of the solar neutrino problem. United States. https://doi.org/10.1103/PhysRevD.53.1665
Krastev, P I, and Petcov, S T. Thu . "Vacuum oscillation solutions of the solar neutrino problem". United States. https://doi.org/10.1103/PhysRevD.53.1665.
@article{osti_282786,
title = {Vacuum oscillation solutions of the solar neutrino problem},
author = {Krastev, P I and Petcov, S T},
abstractNote = {We study the stability of the two-neutrino vacuum oscillation solution of the solar neutrino problem with respect to changes of the total fluxes of {sup 8}B and {sup 7}Be neutrinos, {Phi}{sub B} and {Phi}{sub B}{sub e}. For any value of {Phi}{sub B}{sub e} from the interval 0.7{Phi}{sub B}{sub e}{sup B}{sup P}{le}{Phi}{sub B}{sub e}{le}1.3{Phi}{sub B}{sub e}{sup B}{sup P} the solar {nu}{sub {ital e}} oscillations into an active neutrino, {nu}{sub {ital e}}{leftrightarrow}{nu}{sub {mu}}{sub (}{sub {tau}}{sub )}, provide at 95{percent} C.L. a description of the existing solar neutrino data for {Phi}{sub B}{approx_equal}(0.35{endash}3.4){Phi}{sub B}{sup B}{sup P}, {Phi}{sub B}{sup B}{sup P} and {Phi}{sub B}{sub e}{sup B}{sup P} being the fluxes in the solar model of Bahcall and Pinsonneault from 1992. For {Phi}{sub B}{sub e}{approx_equal}(0.7-1.3){Phi}{sub B}{sub e}{sup B}{sup P} we find also at 95- C.L. two new [one new] {nu}{sub {ital e}}{leftrightarrow}{nu}{sub {mu}}{sub (}{sub {tau}}{sub )} [{nu}{sub {ital e}}{leftrightarrow}{nu}{sub {ital s}}] oscillation solutions: (i) for {Phi}{sub B}{approx_equal}(0.35-0.43){Phi}{sub B}{sup B}{sup P} at {Delta}{ital m}{sup 2}{approx_equal}(4.7-6.5){times}10{sup {minus}}{sup 1}{sup 2} eV{sup 2} [(4.8-6.4){times}10{sup {minus}}{sup 1}{sup 2} eV{sup 2}] and sin{sup 2}2{theta}{approx_gt}0.71[0.74], and (ii) for {Phi}{sub B}{approx_equal}(0.45{endash}0.65){Phi}{sub B}{sup B}{sup P} at {Delta}{ital m}{sup 2}{approx_equal}(3.2-4.0){times}10{sup {minus}}{sup 1}{sup 1} eV{sup 2} and sin{sup 2}2{theta}{approx_gt}0.59. The physical implications of the new solutions for the future solar neutrino experiments are discussed. The data rule out at 97%-98%[99] C.L. the possibility of a universal (neutrino energy independent) suppression of the different components of the solar neutrino flux, resulting from solar {nu}{sub {ital e}} oscillations or transitions into active (sterile) neutrino. {copyright} {ital 1996 The American Physical Society.}},
doi = {10.1103/PhysRevD.53.1665},
url = {https://www.osti.gov/biblio/282786}, journal = {Physical Review, D},
number = 3,
volume = 53,
place = {United States},
year = {1996},
month = {2}
}