A short travel for neutrinos in Large Extra Dimensions

Abstract

Neutrino oscillations successfully explain the flavor transitions observed in neutrinos produced in natural sources like the center of the sun and the earth atmosphere, and also from man-made sources like reactors and accelerators. These oscillations are driven by two mass-squared differences, solar and atmospheric, at the sub-eV scale. However, longstanding anomalies at short-baselines might imply the existence of new oscillation frequencies at the eV-scale and the possibility of this sterile state(s) to mix with the three active neutrinos. One of the many future neutrino programs that are expected to provide a final word on this issue is the Short-Baseline Neutrino Program (SBN) at FERMILAB. In this letter, we consider a specific model of Large Extra Dimensions (LED) which provides interesting signatures of oscillation of extra sterile states. We started re-creating sensitivity analyses for sterile neutrinos in the 3+1 scenario, previously done by the SBN collaboration, by simulating neutrino events in the three SBN detectors from both muon neutrino disappearance and electron neutrino appearance. Then, we implemented neutrino oscillations as predicted in the LED model and also we have performed sensitivity analysis to the LED parameters. Finally, we studied the SBN power of discriminating between the two models, the 3+1 and the LED. We have found that SBN is sensitive to the oscillations predicted in the LED model and have the potential to constrain the LED parameter space better than any other oscillation experiment, for m D 1 < 0.1 eV. In case SBN observes a departure from the three active neutrino framework, it also has the power of discriminating between sterile oscillations predicted in the 3+1 framework and the LED ones.

On The Decaying-Sterile Neutrino Solution to the Electron (Anti)Neutrino Appearance Anomalies

“…The relevant details regarding the three detectors, the flux, the scattering cross-sections and efficiencies are described in Ref. [41] and the assumptions we make here are the same. We are considering only the ν e -appearance channel in order to estimate the sensitivity of the SBN Program.…”

Short-baseline oscillation scenarios at JUNO and TAO

“…Here, E and L are the neutrino energy and the distance traveled by the neutrino. From this formula it becomes clear that the standard mass splittings, characterizing the solar and atmospheric oscillations are given by [43][44][45][46]…”

“…Neutrino oscillations with Large Extra Dimensions have been studied in the context of solar [39], atmospheric [47], accelerator [44][45][46][48][49][50] and reactor neutrinos [51][52][53]. Interestingly, in Ref.…”

On the decaying-sterile-neutrino solution to the electron (anti)neutrino appearance anomalies

“…The relevant details regarding the flux, the scattering cross-sections and efficiencies at the detectors are described in ref. [46] and the assumptions we make here are the same. We are considering only the ν e -appearance channel in order to estimate the sensitivity of the SBN Program.…”

“…Detailed descriptions of the signal and background for the appearance channel can also be found in ref. [46]. The sensitivity of the SBN Program, assuming 6.6 × 10 20 POT for SBND and ICARUS (three nominal years of running) and 1.32 × 10 21 POT for MicroBooNE (six nominal years of running), is depicted in figure 8.…”