Abstract
The relatively large value of neutrino mixing angle \theta_{13} set by recent measurements allows us to use solar neutrinos to set a limit on neutrino magnetic moment involving second and third families, \mu_{\mu\tau}. The existence of a random magnetic field in solar convective zone can produce a significant anti-neutrino flux when a non-vanishing neutrino magnetic moment is assumed. Even if we consider a vanishing neutrino magnetic moment involving the first family, electron anti-neutrinos are indirectly produced through the mixing between first and third families and non-vanishing \mu_{\mu\tau}. Using KamLAND limits on the solar flux of electron anti-neutrino, we set the limit \mu_{\mu\tau} < 0.5e-11 Bohr magneton for a reasonable assumption on the behavior of solar magnetic fields. This is the first time a limit on \mu_{\mu\tau} is established in the literature directly from neutrino interaction with magnetic fields, and, interestingly enough, is comparable with the limits on neutrino magnetic moment involving the first family and with the ones coming from modifications on electroweak cross section.
Highlights
In a recent paper [1] we performed an analysis of how a nonvanishing neutrino transition magnetic moment involving the second and third families, μ23, could affect the flavor conversion of solar neutrinos
At that time we assumed a vanishing θ13, which allowed to produce a large flux of nonelectronic antineutrinos, and our model was not limited by the absence of electron antineutrinos νe in the solar neutrino flux, as required by KamLAND [2]
In that paper it was argued that a nonvanishing θ13 would open a channel for the production of electron antineutrinos, and a limit on μ23 could be established from the absence of a signal of νe in the solar neutrino flux
Summary
In a recent paper [1] we performed an analysis of how a nonvanishing neutrino transition magnetic moment involving the second and third families, μ23, could affect the flavor conversion of solar neutrinos. At that time we assumed a vanishing θ13, which allowed to produce a large flux of nonelectronic antineutrinos, and our model was not limited by the absence of electron antineutrinos νe in the solar neutrino flux, as required by KamLAND [2]. In that paper it was argued that a nonvanishing θ13 would open a channel for the production of electron antineutrinos, and a limit on μ23 could be established from the absence of a signal of νe in the solar neutrino flux. Since recent data indicates a relatively large value for this angle, we examine such limits in light of these new measurements
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