Abstract
We have searched for exotic neutrino-electron interactions that could be produced by a neutrino millicharge, by a neutrino magnetic moment, or by dark photons using solar neutrinos in the XMASS-I liquid xenon detector. We observed no significant signals in 711 days of data. We obtain an upper limit for neutrino millicharge of 5.4×10−12e at 90% confidence level assuming all three species of neutrino have common millicharge. We also set flavor-dependent limits assuming the respective neutrino flavor is the only one carrying a millicharge, 7.3×10−12e for νe, 1.1×10−11e for νμ, and 1.1×10−11e for ντ. These limits are the most stringent yet obtained from direct measurements. We also obtain an upper limit for the neutrino magnetic moment of 1.8×10−10 Bohr magnetons. In addition, we obtain upper limits for the coupling constant of dark photons in the U(1)B−L model of 1.3×10−6 if the dark photon mass is 1×10−3 MeV/c2, and 8.8×10−5 if it is 10 MeV/c2.
Highlights
Liquid xenon (LXe) detectors continue to set stringent limits on weakly interacting massive particle (WIMP) dark-matter models [1, 2, 3, 4]
In the process of an interaction between a neutrino and an electron mediated by a neutrino magnetic moment [25] or by a dark photon from the U (1)B−L model [21], the total number of events Ntot is given by integrating the differential rate in free electron approximation: dNtot =t × N dT ×
The results of our neutrino magnetic moment and dark photon analyses based on free electron approximation (FEA) are conservative relative to what would be expected for relativistic random phase approximation (RRPA)
Summary
Liquid xenon (LXe) detectors continue to set stringent limits on weakly interacting massive particle (WIMP) dark-matter models [1, 2, 3, 4]. We search for interactions between these abundant low energy solar neutrinos and the electrons in the detector’s LXe target that could be signatures of a neutrino electromagnetic millicharge, a neutrino magnetic moment, or interactions mediated by dark photons. The limit in [11] and the second most stringent one, 2.1 × 10−12e [12], were both obtained using reactor neutrinos, meaning electron antineutrinos, and containing negligible amounts of other neutrino species such as νμ and ντ. The dark photon model with U(1)B−L is one of the candidates for explaining the muon g − 2 anomaly if the dark photon mass is O(1 ∼ 1000) keV/c2 with gB−L ∼ O(10−4 ∼ 10−3) [22] These considerations motivate us in our search for exotic neutrino interactions. Since solar neutrinos provide the largest available flux, we used them to search for exotic neutrino interactions with the XMASS-I detector
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