Abstract
The low-energy threshold and the large detector size of Precision IceCube Next Generation Upgrade (PINGU) can make the study on neutrino oscillations with a planet-scale baseline possible. In this task, we consider the configuration that neutrinos are produced at CERN and detected in the PINGU detector, as a benchmark. We discuss its sensitivity of measuring the size of non-standard interactions (NSIs) in matter, which can be described by the parameter $\epsilon_{\alpha\beta}$ ($\alpha$ and $\beta$ are flavors of neutrinos). We find that the CERN-PINGU configuration improves $\tilde{\epsilon}_{\mu\mu}\equiv\epsilon_{\mu\mu}-\epsilon_{\tau\tau}$ and $\epsilon_{\mu\tau}$ significantly compared to the next-generation accelerator neutrino experiments. Most of degeneracy problems in the precision measurements can be resolved, except the one for $\tilde{\epsilon}_{\mu\mu}\sim-0.035$. Moreover, we point out that this configuration can also be used to detect the CP violation brought by NSIs. Finally, we compare the physics potential in this configuration to that for DUNE, T2HK and P2O, and find that the CERN-PINGU configuration can significantly improve the sensitivity to NSIs.
Highlights
Since confirming this phenomenon of neutrino oscillations in 1998 [1], we nearly complete the knowledge of this flavor-changing behavior, which can be described by six oscillation parameters including three mixing angles θ12, θ13 and θ23, two mass-square differences Δm221 and Δm231, and one Dirac CP violating phase δ with solar, atmospheric, accelerator, and reactor neutrino data [2,3,4]
These problems are expected to be resolved in the next-generation neutrino oscillation experiments, e.g., Deep Underground Neutrino Experiment (DUNE), T2HK, JUNO, etc
The neutrino oscillation reflects the fact that neutrinos are massive, which conflicts with the massless-neutrino prediction in the standard model (SM)
Summary
Since confirming this phenomenon of neutrino oscillations in 1998 [1], we nearly complete the knowledge of this flavor-changing behavior, which can be described by six oscillation parameters including three mixing angles θ12, θ13 and θ23, two mass-square differences Δm221 and Δm231, and one Dirac CP violating phase δ with solar, atmospheric, accelerator, and reactor neutrino data [2,3,4]. The large-mixing-angle dark solution (LMA-dark solution) for NSIs allows that NSI matter effects have a strong impact on neutrino oscillations This solution predicts εee ≃ −3 [12,14]. Impacts of NSI matter effects on the precision measurement of oscillation parameters and the expected constraints on. We study the planet-scale neutrino oscillations to measure the size of NSI matter effects, by revisiting the configuration of sending a neutrino beam from an accelerator facility in the northern hemisphere such as CERN to a detector in the south pole like PINGU. Smaller systematic errors and the higher ratio of signals over backgrounds are expected This super long baseline has four advantages for εαβ measurements as follows.
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