KamLAND bounds on solar antineutrinos and neutrino transition magnetic moments

2003/02/28 by E. Torrente-Lujan, E. Torrente-Luján · 1 citation
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Condensed matter physics #Electron #Electron neutrino #Field (mathematics) #Magnetic field #Magnetic moment #Neutrino #Neutrino Physics Research #Neutrino oscillation #Nuclear physics #Order (exchange) #Particle physics #Particle physics theoretical and experimental studies #Physics #Quantum mechanics #Solar neutrino #Spin (aerodynamics) #hep-ph

paper · pdf · doi:10.1088/1126-6708/2003/04/054

published as JHEP 0304:054,2003 · 13 pages, 2 figures

openalex publication_date 2003/04/29 · arxiv created 2003/05/22 · arxiv updated 2014/11/17 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

We investigate the possibility of detecting solar electron antineutrinos with the KamLAND experiment. These electron antineutrinos are predicted by spin-flavor oscillations at a significant rate even if this mechanism is not the leading solution to the SNP. KamLAND is sensitive to antineutrinos originated from solar ⁸B neutrinos. From KamLAND negative results after 145 days of data taking, we obtain model independent limits on the total flux of solar electron antineutrinos Φ(⁸ B)< 1.1-3.5× 10⁴ cm^-2 s^-1, more than one order of magnitude smaller than existing limits, and on their appearance probability P<0.15% (95% CL). Assuming a concrete model for antineutrino production by spin-flavor precession, this upper bound implies an upper limit on the product of the intrinsic neutrino magnetic moment and the value of the solar magnetic field μB< 2.3× 10^-21 MeV 95% CL (for LMA (Δm², tan²θ) values). Limits on neutrino transition moments are also obtained. For realistic values of other astrophysical solar parameters these upper limits would imply that the neutrino magnetic moment is constrained to be, in the most conservative case, μ\lsim 3.9× 10^-12 μ_B (95% CL) for a relatively small field B= 50 kG. For higher values of the magnetic field we obtain: μ\lsim 9.0× 10^-13 μ_B for field B= 200 kG and μ\lsim 2.0× 10^-13 μ_B for field B= 1000 kG at the same statistical significance.

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Cited by

• LMA and sterile neutrinos: a case for resonance spin flavour precession