Study of solar neutrinos with the 600 t liquid argon ICARUS detector

Arneodo, F.; Badertscher, A.; Baibussinov, S; Benetti, P.; Tigliole, A. Borio di; Brunetti, R.; Bueno, A.; Calligarich, E.; Campanelli, M.; Carpanese, C.; Cavalli, D.; Cavanna, F.; Cennini, P.; Centro, S.; Cesana, A.; Chen, C; Chen, Y; Cline, D.; Mitri, I. De; Dolfini, R.; Ferrari, A.; Berzolari, A. Gigli; Goudsmit, P.F.A.; He, K. L.; Li, Z; Lu, F.; Ma, Jin; Mannocchi, G.; Maris, M.; Mauri, F.; Mazza, Davide; Mazzone, L.; Montanari, C.; Otwinowski, S.; Palamara, O.; Pascoli, D.; Pepato, A.; Periale, L.; Petrera, S.; Mortari, G. Piano; Piazzoli, A.; Picchi, P.; Pietropaolo, F.; Rappoldi, A.; Revol, J. P.; Rossella, M.; Rossi, C.; Rubbia, A.; Rubbia, C.; Sala, P.; Scannicchio, D. A.; Sergiampietri, F.; Suzuki, S.; Terrani, M.; Ventura, S.; Vignoli, C.; Wang, H; Woo, J.; Xu, G. F.; Xu, Z.; Zhang, C; Zhang, Q; Zheng, S X

doi:10.1016/s0168-9002(00)00520-9

Cited by 9 publications

(14 citation statements)

References 12 publications

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“…We expect that betas and gammas from intrinsic radioactivities [29] can be mitigated effectively, leaving a negligible rate inside the fiducial volume and above 5 MeV. These long-lived radioactivities have low energies, but can effectively reach higher energies if their rate is high and/or the energy resolution is poor.…”

Section: Appendix B Backgroundsmentioning

confidence: 99%

“…For angular resolution, though we assumed a smearing of 25 • , following ICARUS [29], we conservatively defined the forward cone to have a half-angle of 40 • . Further, we find that the results are not sensitive to reasonable variations from this.…”

Section: D2 Assumed Detector Propertiesmentioning

confidence: 99%

“…We propose that DUNE -intended to make transformative studies of high-energy long-baseline neutrino mixing, proton decay, and supernova neutrino bursts [25][26][27] -has the potential to do the same for solar neutrinos. Building on prior work on solar-neutrino detection in liquid argon [28][29][30][31], our paper goes much further. The budgeted plans for DUNE provide a large active volume, a huge overburden, and excellent technical capabilities, including at MeV energies (for supernova neutrinos) [25][26][27].…”

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confidence: 99%

“…For solar signals, electrons lose energy dominantly by ionization, as the critical energy of LAr is 32 MeV [45][46][47]. The angular resolution of DUNE is uncertain, so we adopt simulation results for ICARUS [29], with a smearing of ∼ 25 • . We present signal and background spectra calculated with conservative assumptions.…”

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confidence: 99%

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DUNE as the Next-Generation Solar Neutrino Experiment

et al. 2019

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We show that the Deep Underground Neutrino Experiment (DUNE) has the potential to deliver world-leading results in solar neutrinos. Significant but realistic new efforts would be required. With an exposure of 100 kton-year, DUNE could detect 10 5 signal events above 5 MeV. Separate precision measurements of neutrino-mixing parameters and the 8 B flux could be made using two detection channels (νe + 40 Ar and νe,µ,τ + e − ) and the day-night effect (> 10σ). New particle physics may be revealed through the comparison of solar neutrinos (with matter effects) and reactor neutrinos (without), which is discrepant by ∼ 2σ (and could become 5.6σ). New astrophysics may be revealed through the most precise measurement of the 8 B flux (to 2.5%) and the first detection of the hep flux (to 11%). DUNE is required: No other experiment, even proposed, has been shown capable of fully realizing these discovery opportunities.12 θ 2 sin 0.2 0.3 0.4

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Section: Appendix B Backgroundsmentioning

confidence: 99%

Section: D2 Assumed Detector Propertiesmentioning

confidence: 99%

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confidence: 99%

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confidence: 99%

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DUNE as the Next-Generation Solar Neutrino Experiment

et al. 2019

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“…There are important differences in the signal detection technique: the water Cherenkov signal detection is through elastic scattering of neutrinos off electrons whereas in liquid argon there is expectation that absorption of neutrinos on 40 Ar will be dominant. The event rates from elastic scattering and absorption on 40 Ar are expected to be in the ratio of 1:∼3 in a liquid argon detector, but the exact ratio depends on the energy threshold [20]. Nevertheless, it is clear that the depth requirements for a water detector are applicable to a liquid argon detector as well.…”

Section: Fig 10: Spallation Induced Deadtime Versus Depth In Solar Nmentioning

confidence: 99%

Report on the Depth Requirements for a Massive Detector at Homestake

Bernstein¹,

Bishai²,

Blucher³

et al. 2008

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This report provides the technical justification for locating a large detector underground in a US based Deep Underground Science and Engineering Laboratory. A large detector with a fiducial mass greater than 100 kTon will most likely be a multipurpose facility. The main physics justification for such a device is detection of accelerator generated neutrinos, nucleon decay, and natural sources of neutrinos such as solar, atmospheric and supernova neutrinos. The requirement on the depth of this detector will be guided by the rate of signals from these sources and the rate of backgrounds from cosmic rays over a very wide range of energies (from solar neutrino energies of 5 MeV to high energies in the range of tens of GeV).For the present report, we have examined the depth requirement for a large water Cherenkov detector and a liquid argon time projection chamber. There has been extensive previous experience with underground water Cherenkov detectors such as IMB, Kamioka, and most recently, Super-Kamiokande which has a fiducial mass of 22 kTon and a total mass of 50 kTon at a depth of 2700 meters-water-equivalent. Projections for signal and background capability for a larger and deeper (or shallower) detectors of this type can be scaled from these previous detectors. The liquid argon time projection chamber has the advantage of being a very fine-grained tracking detector, which provides enhanced capability for background rejection.In the current work we have taken the approach that the depth should be sufficient to suppress the cosmogenic background below predicted signal rates for either of the above two technologies. Nevertheless, it is also clear that the underground facility that we are examining must have a long life and will most likely be used either for future novel uses of the currently planned detectors or new technologies. Therefore the depth requirement also needs to be made on the basis of sound judgment regarding possible future use. In particular, the depth should be sufficient for any possible future use of these cavities or the level which will be developed for these large structures.Along with these physics justifications there are practical issues regarding the existing infrastructure at Homestake and also the stress characteristics of the Homestake rock formations. In this report we will examine the various depth choices at Homestake from the point of view of the particle and nuclear physics signatures of interest. We also have sufficient information about the existing infrastructure and the rock characteristics to narrow the choice of levels for the development of large cavities with long lifetimes. We make general remarks on desirable ground conditions for such large cavities and then make recommendations on how to start examining these levels to make a final choice. In the appendix we have outlined the initial requirements for the detectors. These requirements will undergo refinement during the course of the design. Finally, we strongly recommend that the geotechnical studies be commen...

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Solar neutrino physics: Historical evolution, present status and perspectives

Miramonti

Reseghetti

2002

Riv. Nuovo Cim.

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Solar neutrino physics is an exciting and difficult field of research for physicists, where astrophysics, elementary particle and nuclear physics meet. The Sun produces the energy that life has been using on Earth for many years, about 10 9 y, emits a lot of particles: protons, electrons, ions, electromagnetic quanta... among them neutrinos play an important role allowing to us to check our knowledge on solar characteristics. The main aim of this paper is to offer a practical overview of various aspects concerning the solar neutrino physics: after a short historical excursus, the different detection techniques and present experimental results and problems are analysed. Moreover, the status of art of solar modeling, possible solutions to the so called solar neutrino problem (SNP) and planned detectors are reviewed.

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Study of solar neutrinos with the 600 t liquid argon ICARUS detector

Cited by 9 publications

References 12 publications

DUNE as the Next-Generation Solar Neutrino Experiment

DUNE as the Next-Generation Solar Neutrino Experiment

Report on the Depth Requirements for a Massive Detector at Homestake

Solar neutrino physics: Historical evolution, present status and perspectives

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