JUNO physics and detector
JUNO; neutrino physics; neutrino detector;
neutrino p: elastic scattering
neutrino: solar
particle identification: efficiency
scintillation counter: liquid
energy resolution
7. Clean energy
01 natural sciences
photon: particle identification
JUNO; neutrino detector; neutrino physics
High Energy Physics - Experiment
High Energy Physics - Experiment (hep-ex)
JUNO; neutrino physics; neutrino detector
[PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex]
neutrino: supernova
neutrino: mass
p: lifetime: lower limit
membrane
JUNO
photomultiplier
electronics
radon
neutrino electron: elastic scattering
observatory
neutrino: detector
neutrino detector
neutrino: geophysics
numerical calculations: Monte Carlo
performance
[PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex]
JUNO; neutrino detector; neutrino physics;
water
neutrino: mass difference
review
FOS: Physical sciences
fabrication
530
near detector
neutrino physics
0103 physical sciences
calorimeter
antineutrino: nuclear reactor
activity report
detector: design
p --> antineutrino K+
neutrino: mixing angle
deep underground detector
attenuation: length
13. Climate action
efficiency
neutrino: oscillation
experimental results
DOI:
10.1016/j.ppnp.2021.103927
Publication Date:
2021-12-03T12:26:02Z
AUTHORS (256)
ABSTRACT
A review paper with 78 pages and 32 figures. v2: minor revision. Final version to appear in Progress in Particle and Nuclear Physics<br/>The Jiangmen Underground Neutrino Observatory (JUNO) is a 20 kton LS detector at 700-m underground. An excellent energy resolution and a large fiducial volume offer exciting opportunities for addressing many important topics in neutrino and astro-particle physics. With 6 years of data, the neutrino mass ordering can be determined at 3-4 sigma and three oscillation parameters can be measured to a precision of 0.6% or better by detecting reactor antineutrinos. With 10 years of data, DSNB could be observed at 3-sigma; a lower limit of the proton lifetime of 8.34e33 years (90% C.L.) can be set by searching for p->nu_bar K^+; detection of solar neutrinos would shed new light on the solar metallicity problem and examine the vacuum-matter transition region. A core-collapse supernova at 10 kpc would lead to ~5000 IBD and ~2000 (300) all-flavor neutrino-proton (electron) scattering events. Geo-neutrinos can be detected with a rate of ~400 events/year. We also summarize the final design of the JUNO detector and the key R&D achievements. All 20-inch PMTs have been tested. The average photon detection efficiency is 28.9% for the 15,000 MCP PMTs and 28.1% for the 5,000 dynode PMTs, higher than the JUNO requirement of 27%. Together with the >20 m attenuation length of LS, we expect a yield of 1345 p.e. per MeV and an effective energy resolution of 3.02%/\sqrt{E (MeV)}$ in simulations. The underwater electronics is designed to have a loss rate <0.5% in 6 years. With degassing membranes and a micro-bubble system, the radon concentration in the 35-kton water pool could be lowered to <10 mBq/m^3. Acrylic panels of radiopurity <0.5 ppt U/Th are produced. The 20-kton LS will be purified onsite. Singles in the fiducial volume can be controlled to ~10 Hz. The JUNO experiment also features a double calorimeter system with 25,600 3-inch PMTs, a LS testing facility OSIRIS, and a near detector TAO.<br/>
SUPPLEMENTAL MATERIAL
Coming soon ....
REFERENCES (232)
CITATIONS (166)
EXTERNAL LINKS
PlumX Metrics
RECOMMENDATIONS
FAIR ASSESSMENT
Coming soon ....
JUPYTER LAB
Coming soon ....