Science and technology of Borexino: a real-time detector for low energy solar neutrinos

Alimonti, G.; Arpesella, C.; Back, H. O.; Balata, M.; Beau, T.; Bellini, G.; Benziger, J.; Bonetti, S.; Brigatti, A.; Caccianiga, B.; Cadonati, L.; Calaprice, F.; Cecchet, G.; Chen, M.; Bari, A. de; Haas, E. de; Kerret, H. de; Donghi, O.; Deutsch, Martin; Elisei, Fausto; Etenko, A.; Feilitzsch, F. von; Fernholz, Robert; Ford, R.; Freudiger, B.; Garagiola, A.; Galbiati, C.; Gatti, F.; Gazzana, S.; Giammarchi, M.; Giugni, D.; Golubchikov, A.; Goretti, A.; Grieb, C.; Hagner, C.; Hagner, T.; Hampel, W.; Harding, Eric; Hartmann, F.; Hentig, R. von; Hess, H.; Heusser, G.; Ianni, Aldo; Inzani, P.; Kidner, S.; Kiko, J.; Kirsten, T.; Korga, G.; Korschinek, G.; Kryn, D.; Lagomarsino, V.; LaMarche, P. H.; Laubenstein, M.; Loeser, F.; Lombardi, P.; Magni, Stefano; Malvezzi, S.; Maneira, J.; Manno, I.; Manuzio, G.; Masetti, F.; Mazzucato, U.; Meroni, E.; Musico, P.; Neder, H.; Neff, M.; Nisi, S.; Oberauer, L.; Obolensky, M.; Pallavicini, M.; Papp, L.; Perasso, L.; Pocar, A.; Raghavan, R. S.; Ranucci, G.; Rau, W.; Razeto, A.; Resconi, E.; Riedel, Timothy E.; Sabelnikov, A.; Salvo, C.; Scardaoni, R.; Schönert, S.; Schuhbeck, K. H.; Shutt, T.; Simgen, H.; Sonnenschein, A.; Smirnov, O.; Sotnikov, A.; Skorokhvatov, M.; Sukhotin, S.; Tartaglia, R.; Testera, G.; Vogelaar, R. B.; Vitale, S.; Wójcik, Marcin; Zaimidoroga, O.; Zakharov, Yu. I.

doi:10.1016/s0927-6505(01)00110-4

Cited by 338 publications

(416 citation statements)

References 58 publications

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“…ref. [10]). For simplicity in presentation and following the general practice in the literature, we refer to these events as 7 Be neutrino events.…”

Section: Predictions For 7 Be Rate and Day-night Effectmentioning

confidence: 99%

“…For the Sudbury Neutrino Observatory (SNO) [7,9], we report the predictions of the currently allowed regions for the neutral current to charged current double ratio, [NC]/[CC], the daynight effect, and the first and second moments of the electron recoil energy spectrum. For experiments like BOREXINO [10] and KamLAND [11] that can detect 7 Be solar neutrinos, we evaluate the predicted range of the neutrino-electron scattering rate and the difference between the night and the day event rates.…”

Section: Introductionmentioning

confidence: 99%

“…As a number of previous authors have discussed (see, e. g., refs. [10,50,51] and references cited therein), the LOW solution is the only currently allowed oscillation solution that predicts a large night-day difference in the rates. The LMA solution predicts a negligible variation and therefore the 1σ predicted range is effectively zero.…”

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confidence: 99%

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Robust signatures of solar neutrino oscillation solutions

Bahcall

González-García

Peña-Garay

2002

J. High Energy Phys.

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With the goal of identifying signatures that select specific neutrino oscillation parameters, we test the robustness of global oscillation solutions that fit all the available solar and reactor experimental data. We use three global analysis strategies previously applied by different authors and also determine the sensitivity of the oscillation solutions to the critical nuclear fusion cross section, S 17 (0), for the production of 8 B. Our standard results make use of the precise new measurement of S 17 (0) by Junghans et al. The globally favored solutions are, in order of goodness of fit: LMA(the only solution at 2σ), LOW, and VAC. The NC to CC ratio for SNO is predicted by the standard global analysis to be 3.45 +0.70 −0.54 (1σ) which is separated from the no-oscillation value of 1.0 by much more than the expected experimental error. The predicted range of the day-night difference in CC rates is 8.3 +5.0 −5.6 (1σ)%. A measurement by SNO of either a NC to CC ratio > 3.3 or a day-night difference > 10%, would favor a small region of the currently allowed LMA neutrino parameter space. The global oscillation solution predicts a 7 Be neutrino-electron scattering rate in BOREXINO and KamLAND in the range 0.65 +0.04 −0.03 (1σ) of the BP00 standard solar model rate, a prediction which can be used to test both the solar model and the neutrino oscillation theory. Only the LOW solution predicts a large day-night effect(≤ 42%, 3σ) in BOREXINO and KamLAND. For the reactor KamLAND experiment, the LMA solution predicts a charged current rate relative to the standard model of 0.44 +0.22 −0.07 (1σ), E threshold = 1.22 MeV. We have also evaluated the effects of including preliminary Super-Kamiokande data for 1496 days of observations.

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“…ref. [10]). For simplicity in presentation and following the general practice in the literature, we refer to these events as 7 Be neutrino events.…”

Section: Predictions For 7 Be Rate and Day-night Effectmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Robust signatures of solar neutrino oscillation solutions

Bahcall

González-García

Peña-Garay

2002

J. High Energy Phys.

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“…The forthcoming neutrino experiments Borexino [29] and Kamland [30] will be crucial to test the validity of the RSFP hypothesis against oscillations. In fact, at the present stage both the LMA and RSFP solutions give global fits of equally good quality and, as far as rates only are concerned, RSFP solutions provide the best of all fits.…”

Section: Discussionmentioning

confidence: 99%

Solar neutrinos with magnetic moment: rates and global analysis

Pulido¹

2002

Astroparticle Physics

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A statistical analysis of the solar neutrino data is presented assuming the solar neutrino deficit to be resolved by the resonant interaction of the neutrino magnetic moment with the solar magnetic field. Four field profiles are investigated, all exhibiting a rapid increase across the bottom of the convective zone, one of them closely following the requirements from recent solar physics investigations. First a 'rates only' analysis is performed whose best fits appear to be remarkably better than all fits from oscillations. A global analysis then follows with the corresponding best fits of a comparable quality to the LMA one. Despite the fact that the resonant spin flavour precession does not predict any day/night effect, the separate SuperKamiokande day and night data are included in the analysis in order to allow for a direct comparison with oscillation scenarios. Remarkably enough, the best fit for rates and global analysis which is compatible with most astrophysical bounds on the neutrino magnetic moment is obtained from the profile which most closely follows solar physics requirements. Allowing for a peak field value of 3 × 10 5 G, it is found in this case that ∆m 2 21 = 1.46 × 10 −8 eV 2 , µ ν = 3.2 × 10 −12 µ B (64%CL). The new forthcoming experiments on solar neutrino physics (Kamland and Borexino) will be essential to ascertain whether this fact is incidental or essential. *

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“…The maximum energy of the recoiling electron is 664 keV and the experimental design threshold is set at 250 keV [4].…”

Section: The Borexino Detectormentioning

confidence: 99%

Geoneutrinos in Borexino

Giammarchi

Miramonti

2006

Earth Moon Planet

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Abstract. This paper describes the Borexino detector and the high-radiopurity studies and tests that are integral part of the Borexino technology and development. The application of Borexino to the detection and studies of geoneutrinos is discussed. . The Gran Sasso National LaboratoryThe Gran Sasso National Laboratory (Laboratori Nazionali del Gran Sasso -LNGS), home of the Borexino experiment, is the world's largest underground laboratory. It is located in the center of Italy in the highway tunnel between Teramo and L'Aquila under the "Monte Aquila" (Gran Sasso mountain). The laboratory is financed and operated by the Italian National Institute for Nuclear Physics (Infn). Its total underground volume is about 180,000 m 3 with an area greater than 13500 m 2 . It is composed of three main experimental halls (20 m high, 18 m wide and 100 m long). The overburden rock is on the average about 1,400 m, equivalent to 3,700 meters of water. The muon flux is reduced by about 6 orders of magnitude to a value of approximately 1.1 muons per square meter per hour, whereas the neutron flux is of the order of 3 × 10 −6 neutrons per square centimeter per second with energies greater than 2.5 MeV.The rock of the Gran Sasso mountain has a density of 2.71 ± 0.05 g · cm −3 , and consists mainly of CaCO 3 and M gCO 3 [1]. The primordial radionuclide content of the rock of Hall C is 0.66 ± 0.14 ppm for 238 U, 0.066 ± 0.025 ppm for the 232 Th and 160 ppm for K [2]. The radioactive content of the concrete employed as experimental hall liner is 1.05 ± 0.12 ppm for 238 U and 0.656 ± 0.028 ppm for the 232 Th [3].The LNGS hosts about 15 experiments of astroparticle physiscs such as neutrino research, double beta decay physics, dark matter studies and nuclear astrophysics. Interdisciplinary studies (biology, geology) are also conducted in the LNGS underground location.The Borexino detector is located in one of the big underground experimental halls, hall C. The Borexino detectorBorexino is a real time experiment whose main goal is to study the low energy (sub-MeV) solar neutrinos, and in particular the 862 keV 7 Be solar neutrino line, through the neutrino-electron elastic scattering reaction. The maximum energy of the recoiling electron is 664 keV and the experimental design threshold is set at 250 keV [4].

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Science and technology of Borexino: a real-time detector for low energy solar neutrinos

Cited by 338 publications

References 58 publications

Robust signatures of solar neutrino oscillation solutions

Robust signatures of solar neutrino oscillation solutions

Solar neutrinos with magnetic moment: rates and global analysis

Geoneutrinos in Borexino

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