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Physics with JUNO

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Physics with JUNO Physics with JUNO CNRS/IN2P3 2020 Prospect on Neutrino Physics J. P. Athayde Marcondes de Andr´e3, E. Baussan3, T. J. C. Bezerra5, J. Busto2, M. Bongrand4, A. Cabrera∗4, C. Cerna1, M. Dracos3, C. Jollet1, L. N. Kalousis3, F. Perrot1, A. Meregaglia1, M. Settimo5, B. Viaud5, and F. Yermia5 1CENBG, Universit´ede Bordeaux, CNRS/IN2P3, F-33170, Gradignan, France 2CPPM, Aix Marseille University, CNRS/IN2P3, Marseille, France 3IPHC, Universit´ede Strasbourg, CNRS/IN2P3 , Strasbourg, France 4LAL, Univ. Paris-Sud, CNRS/IN2P3, Universit´eParis-Saclay, Orsay, France 5SUBATECH, CNRS/IN2P3, Universit´ede Nantes, IMT-Atlantique, 44307 Nantes, France September 20, 2019 Reactor neutrinos have been an important class of experiments for both discovery and precision measurement in the history of neutrino studies. Since the first generation of reactor neutrino experiments in the 1950s with Reines and Cowan, the detector technology has greatly advanced. The current experiments, Daya Bay, Double Chooz and RENO have led neutrino physics into the precision era (a few %). The Jiangmen Underground Neutrino Observatory (JUNO) is designed to study neutrino mass ordering and measure three of the neutrino oscillation parameters with high precision (towards sub-percent) using reactor neutrinos. Many other physical phenomena, including supernova neutrinos, solar neutrinos, geo-neutrinos, atmospheric neutrinos can be studied with JUNO through differents detection channels. The CNRS/IN2P3 teams involved in the JUNO experiment here highlight the JUNO potential for physics in terms of possible impact and synergy to other research fields. Preamble open questions of neutrino physics. JUNO will look at the oscillation frequencies at the first oscillation maxi- 2 The Jiangmen Underground Neutrino Observatory mum defined by θ12 and ∆m21, where the discrimination (JUNO)[1] is a 20 kton multi-purpose underground for the MO choice is enhanced. To determine the MO, liquid scintillator detector, similar to KamLAND and JUNO aims to resolve the neutrino spectrum wiggles 2 Borexino, located in China. Nuclear reactors 53 km (due to θ13 and ∆mee). Indeed, their phase discrimi- far away from the detector, are the neutrino source nates between Normal and Inverted Ordering (NO and for JUNO. The JUNO detector provides the necessary IO). For that purpose, an outstanding 3% energy resolu- size to address simultaneously several important physics tion at 1 MeV must be achieved. It is expected that after challenges. The excellent energy resolution and the large six years of operation, JUNO will reach a sensitivity be- fiducial volume anticipated for the JUNO detector of- tween 3 to 4 σ on the MO determination. Moreover, the fer exciting opportunities for addressing many impor- measurement of the antineutrino spectrum with excel- tant topics in neutrino and astro-particle physics. A lent energy resolution will also lead to the precise deter- 2 non-negligible challenge lays inside the central detec- mination of the neutrino oscillation parameters sin 2θ12, 2 2 tor, surrounded by muon detectors (a Top Tracker and ∆m21, and ∆mee to an accuracy better than 1%, which a water Cherenkov Outer Veto). The target volume, will play a crucial role in the future unitarity test of the where neutrinos detection takes place, is read out by a PMNS matrix. JUNO will obverse for the first time the 2 double PMT system, using 18,000 20" PMTs (labelled two oscillation patterns, the one lead by ∆m21 and the 2 Large PMT system) and 25,600 3" (labelled Small PMT other by ∆mee, since so far all the experiments observed system) PMTs. The JUNO international collaboration an oscillation pattern that could be approximated by the consists of 77 institutes around the world (600 collabo- two flavor case. The data taking is to start by 2022. rators). One of its purposes is the determination of the neu- trino Mass Ordering (MO), which is one of the main ∗CNRS/IN2P3 Contact: [email protected] and +33 675 388 007. 1 Neutrino Oscillation Physics both the unitarity of the lepton mixing matrix and the relationship between neutrino oscillation frequencies. As discussed before, neutrino oscillations are a core topic All results discussed above will be obtained via the of JUNO. With all recent advances in neutrino oscil- study of reactor electron antineutrino disappearance. In lation measurements in the past decades, we started addition to studying neutrino oscillations using neutri- getting a more complete picture of the neutrino oscil- nos from reactors, JUNO will also be able to probe neu- lations. However, there are mainly two main unknowns: trino oscillations from other neutrino sources. In case the neutrino mass ordering, that is which neutrino is JUNO observes a supernova, it will be possible to make the lightest, and the CP violating phase in the neutrino an independent determination of the neutrino mass or- sector. JUNO will be able to determine the neutrino dering. In this case, the ordering will change how mat- mass ordering with 6 years of data taking with a 3 σ ter affects neutrino oscillations and change the observed significance by itself. Early studies indicate it should neutrino spectra from the supernova. Even if neutrino reach beyond 5 σ significance in combination with other oscillation measurements with these other sources do experiments such as KM3NeT-ORCA [2] and IceCube not reach the precision obtained from reactor antineutri- [3], in a similar time frame. The discovery of the neu- nos, they will still constitute an important verification trino mass ordering will have important phenomenolog- of the consistency of the neutrino oscillation framework, ical consequences for the supernova neutrinos, cosmol- within a single detector. Searches for light sterile neu- ogy as well as for atmospheric and accelerator neutrinos trinos with JUNO will also be possible by augmenting propagating in the matter of the Earth. The ordering the detector by either adding a source to the center of is important whenever the matter effects on oscillations the detector, or by adding a cyclotron-drive source (Iso- are driven by the 1-3 mixing and corresponding mass DAR) located close to JUNO, however their realisation splittings [4]. Its determination may provide the key to will be dependent on results from current light sterile establish the relationship among the lepton masses and neutrino experimental searches. mixing. The extraction of the neutrino mass ordering The CNRS/IN2P3 groups have strong interest in the is a data-driven field expected to evolve very rapidly neutrino oscillation physics, and have previous experi- in the next decade, starting with JUNO and KM3NeT- ence with having performed neutrino oscillation analyses ORCA neutrino experiments. Since neutrino oscillation previously in several different experiments. measurements, cosmological observations and neutrino- less double beta decay experiments are cornering the in- Astrophysics verted mass ordering region, it makes sense to combine their results. In addition, it should help the discovery of With its huge target mass, the low-energy threshold the CP violating phase and serve as guide for neutrino- and the unprecedented energy resolution and energy less double beta decay searches. scale precision, JUNO is a competitive detector for as- Even after the discovery of the neutrino mass order- trophysical programs, such as galactic core-collapse su- ing and the CP violating phase, there will be significant pernova neutrinos (CCSN), diffuse supernova neutrino room for probing the lepton mixing framework, to make background (DSNB) and solar neutrinos. In the CCSN, it as precise as the quark mixing one. Therefore, there a massive star with masses above eight solar masses is is still significant room for new physics. Probing the expected to collapse under its own gravity and then consistency of the lepton mixing framework will require to explode emitting 99% of its binding energy in the high precision measurements of several oscillations pa- form of a neutrino burst [5]. Astrophysical models pre- rameters in order to both check the unitarity of the mix- dict a rate of CCSN of about three per century in our ing matrix and verify the relation between the oscillation galaxy, the last one being in 1987, with a distance dis- frequencies in neutrino mixing. The latter is tied to the tribution peaked in the region of ten kpc (e.g. [6]). At 2 2 2 ∆m32 + ∆m21 = ∆m31 relationship among the neutrino these distances, at least one SN is expected during the mass squared differences. JUNO will be able to measure operation time of JUNO. The precise determination of for the first time both solar and atmospheric neutrino os- the energy spectrum and its flavour and time evolution cillations at the same time using reactor anti-neutrinos. would allow us to infer parameters of interests for as- JUNO will measure with a sub-percent precision for the trophysics, nuclear physics and particle physics (mass first time one mixing angle and the two mass squared ordering, constraints on absolute neutrino masses, ster- differences. While reaching the same level as the checks ile neutrinos or possible new physics). The number of done to the mixing of quarks is still far in the future, events varies between up to millions depending on the JUNO's measurements will be a corner stone for testing SN distance (∼ 6000 at 10 kpc) and the detector will be 2 sensitive to different neutrino (antineutrino) flavors and ties. This is a way to probe physics beyond the Standard interaction channels, the dominant IBD process as well Model (SM). Indeed, in the framework of the SM, no as neutral- and charge-current interactions on 12C and observable baryon number violation is allowed. This is, elastic scattering on electrons and proton [7]. The pos- however, a generic prediction of Grand Unified Theories sible detection of O(100) pre-SN neutrinos would also (GUTs). Among the channels predicted by various mod- be possible and is investigated as valuable warning sys- els, 2 are of particular interest : p ! e+π0 and p ! K+ν¯.
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