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Low-energy electronic recoil caused by solar neutrinos in multi-ton xenondetectors is an important subject not only because it is a source of theirreducible background for direct searches of weakly-interacting massiveparticles (WIMPs), but also because it provides a viable way to measure thesolar $pp$ and $^{7}\textrm{Be}$ neutrinos at the precision level of currentstandard solar model predictions. In this work we perform $\textit{ab initio}$many-body calculations for the structure, photoionization, andneutrino-ionization of xenon. It is found that the atomic binding effect yieldsa sizable suppression to the neutrino-electron scattering cross section at lowrecoil energies. Compared with the previous calculation based on the freeelectron picture, our calculated event rate of electronic recoil in the samedetector configuration is reduced by about $25\%$. We present in this paper theelectronic recoil rate spectrum in the energy window of 100 eV - 30 keV withthe standard per ton per year normalization for xenon detectors, and discussits implication for low energy solar neutrino detection (as the signal) andWIMP search (as a source of background).

Low-energy electronic recoil in xenon detectors by solar neutrinos