KamLAND, solar antineutrinos and the solar magnetic field

Abstract

In this work the possibility of detecting solar electron antineutrinos produced by a solar core magnetic field from the KamLAND recent observations is investigated. We find a scaling of the antineutrino probability with respect to the magnetic field profile in the sense that the same probability function can be reproduced by any profile with a suitable peak field value. In this way the solar electron antineutrino spectrum can be unambiguosly predicted. We use this scaling and the negative results indicated by the KamLAND experiment to obtain upper bounds on the solar electron antineutrino flux. We get ${\varphi }_{\bar{\nu }}<3.8\times 10^{-3}\varphi {(}^{8}B)$ at 95% CL. For 90% CL this becomes ${\varphi }_{\bar{\nu }}<3.4\times 10^{-3}\varphi {(}^{8}B)$, an improvement by a factor of 3-5 with respect to existing bounds. These limits are independent of the detailed structure of the magnetic field in the solar interior. We also derive upper bounds on the peak field value which are uniquely determined for a fixed solar field profile. In the most efficient antineutrino producing case, we get (95% CL) an upper limit on the product of the neutrino magnetic moment by the solar field $\mu B<2.8\times 10^{-19}$ MeV or $B_0\le 4.9\times 10^{7}G$ for ${\mu }_{\nu }=10^{-12}{\mu }_B$.

arXiv comment15 pages. References corrected. Minor changes in the text

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• Neutrino mass parameters from Kamland, SNO and other solar evidence
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