Observation of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">B</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>8</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>solar neutrinos in the Kamiokande-II detector

Ks, Hirata; Kajita, T.; Kifune, T.; Kihara, K.; Nakahata, M.; Nakamura, Kenzo; Ōhara, S.; Oyama, Y.; Sato, Nobuaki; Takita, M.; Totsuka, Y.; Yanagimoto, Yoshitomo; Mori, M.; Suzuki, A.; Takahashi, K.; Tanimori, T.; Yamada, Masashi; Koshiba, M.; Suda, T.; Miyano, K.; Miyata, H.; Takei, H.; Kaneyuki, K.; Nagashima, Hiroki; Suzuki, Y.; Beier, E. W.; Lr, Feldscher; Ed, Frank; Frati, W.; Kim, SB; Ak, Mann; Fm, Newcomer; R, Van Berg; W, Zhang

doi:10.1103/physrevlett.63.16

Cited by 420 publications

(232 citation statements)

References 7 publications

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“…In the 70's and the 80's the Chlorine radiochemical experiment at Homestake [192] and the Cherenkov detector Kamiokande [193] played the fundamental role to establish on solid rock basis what became known as the Solar Neutrino Problem (SNP), i.e. the persisting discrepancy between the measured and predicted solar neutrino flux.…”

Section: Experimental Statusmentioning

confidence: 99%

The next-generation liquid-scintillator neutrino observatory LENA

Wurm

Beacom

Bezrukov

et al. 2012

Astroparticle Physics

212

200

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2As part of the European LAGUNA design study on a next-generation neutrino detector, we propose the liquid-scintillator detector LENA (Low Energy Neutrino Astronomy) as a multipurpose neutrino observatory. The outstanding successes of the Borexino and KamLAND experiments demonstrate the large potential of liquid-scintillator detectors in low-energy neutrino physics. Low energy threshold, good energy resolution and efficient background discrimination are inherent to the liquidscintillator technique. A target mass of 50 kt will offer a substantial increase in detection sensitivity.At low energies, the variety of detection channels available in liquid scintillator will allow for an energy-and flavor-resolved analysis of the neutrino burst emitted by a galactic Supernova. Due to target mass and background conditions, LENA will also be sensitive to the faint signal of the Diffuse Supernova Neutrino Background. Solar metallicity, time-variation in the solar neutrino flux and deviations from MSW-LMA survival probabilities can be investigated based on unprecedented statistics. Low background conditions allow to search for dark matter by observing rare annihilation neutrinos. The large number of events expected for geoneutrinos will give valuable information on the abundances of Uranium and Thorium and their relative ratio in the Earth's crust and mantle. Reactor neutrinos enable a high-precision measurement of solar mixing parameters. A strong radioactive or pion decay-at-rest neutrino source can be placed close to the detector to investigate neutrino oscillations for short distances and sub-MeV to MeV energies.At high energies, LENA will provide a new lifetime limit for the SUSY-favored proton decay mode into kaon and antineutrino, surpassing current experimental limits by about one order of magnitude. Recent studies have demonstrated that a reconstruction of momentum and energy of GeV particles is well feasible in liquid scintillator. Monte Carlo studies on the reconstruction of the complex event topologies found for neutrino interactions at multi-GeV energies have shown promising results. If this is confirmed, LENA might serve as far detector in a long-baseline neutrino oscillation experiment currently investigated in LAGUNA-LBNO.3

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Section: Experimental Statusmentioning

confidence: 99%

The next-generation liquid-scintillator neutrino observatory LENA

Wurm

Beacom

Bezrukov

et al. 2012

Astroparticle Physics

212

200

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“…Solar models have played a particularly important role, in large part because we have powerful diagnostics of the internal solar conditions from solar neutrino experiments and helioseismology. The deficit of the observed solar neutrino fluxes relative to solar model predictions, initially reported by Homestake (Davis et al 1968) and then confirmed by GALLEX/GNO (Hampel et al 1999;Altmann et al 2005), SAGE (Abdurashitov et al 1999), Kamiokande (Hirata et al 1989) and Super-Kamiokande (Cravens et al 2008), SNO (Ahmad et al 2002) and Borexino (Arpesella et al 2008), gave rise to the solar neutrino problem: major changes were required in either the theory of stellar structure and evolution and neutrino physics. The development, refinement, and testing of the Standard Solar Model (SSM) played an important role in its ultimate resolution in 2002 1 , when the SNO experiment obtained direct evidence for flavor oscillations of solar neutrinos and confirmed the SSM prediction of the 8 B neutrino flux with a precision that, according to the latest data, is equal to about 3%.…”

Section: Introductionmentioning

confidence: 99%

The Chemical Composition of the Sun From Helioseismic and Solar Neutrino Data

Villante¹,

Serenelli²,

Delahaye³

et al. 2014

ApJ

145

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We perform a quantitative analysis of the solar composition problem by using a statistical approach that allows us to combine the information provided by helioseimic and solar neutrino data in an effective way. We include in our analysis the helioseismic determinations of the surface helium abundance and of the depth of the convective envelope, the measurements of the 7 Be and 8 B neutrino fluxes, the sound speed profile inferred from helioseismic frequencies. We provide all the ingredients to describe how these quantities depend on the solar surface composition and to evaluate the (correlated) uncertainties in solar model predictions. We include errors sources that are not traditionally considered such as those from inversion of helioseismic data. We, then, apply the proposed approach to infer the chemical composition of the Sun. We show that the opacity profile of the Sun is well constrained by the solar observational properties. In the context of a two parameter analysis in which elements are grouped as volatiles (i.e. C, N, O and Ne) and refractories (i.e Mg, Si, S, Fe), the optimal composition is found by increasing the the abundance of volatiles by (45 ± 4) % and that of refractories by (19 ± 3) % with respect to the values provided by Asplund et al. (2009). This corresponds to the abundances ε O = 8.85 ± 0.01 and ε Fe = 7.52 ± 0.01. As an additional result of our analysis, we show that the observational data prefer values for the input parameters of the standard solar models (radiative opacities, gravitational settling rate, the astrophysical factors S 34 and S 17 ) that differ at the ∼ 1σ level from those presently adopted.

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“…The outgoing e − direction from elastic scattering is correlated to the direction of the neutrinos from the Sun. Kamiokande confirmed the deficit of solar neutrinos [38] and the similar, but much larger Super-Kamiokande (SK), recently measured the same flux [39].…”

Section: Cerenkov Detector Experimentsmentioning

confidence: 56%

Sterile neutrino oscillations in MINOS and hadron production in pC collisions

Tinti

2010

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MINOS is a long baseline neutrino oscillation experiment, starting with a muon-neutrino beam, for the precise measurement of the atmospheric neutrino oscillation parameters |∆m 2 | and θ 23 . The Near Detector measures the neutrino flux and spectra before oscillations. The beam propagates for 735 km to the Far Detector, which measures the depleted spectrum after oscillations. The depletion can be interpreted as ν µ → ν τ oscillations. Subdominant ν µ → ν e oscillations may be allowed if the mixing angle θ 13 = 0.The two detectors are functionally identical in order to cancel systematic errors when using the Near Detector data to constrain the Far Detector prediction. A crucial part of the analysis is the relative calibration between the two detectors, which is known at the 2% level. A calibration procedure to remove the time and temperature dependence of the detector response using through-going cosmic muons is presented here.Although the two-detector approach reduces the systematic uncertainties related to the neutrino flux, a cross check on the neutrino parent meson ratios is performed in this thesis. The cross sections of mesons produced in proton-carbon interactions from the NA49 experiment have been measured and the results have been compared to the MINOS expectations.A neutrino oscillation analysis allowing mixing to a sterile neutrino is performed, under the assumption that the additional mass splitting is O(1 eV 2 ). The analysis uses the energy spectrum of the neutral current interaction products, as neutral current interactions are sensitive to sterile neutrino mixing but not to the active flavour neutrino mixing. The neutrino oscillation parameters have been found to be: To my parents

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Observation ofB8solar neutrinos in the Kamiokande-II detector

Cited by 420 publications

References 7 publications

The next-generation liquid-scintillator neutrino observatory LENA

The next-generation liquid-scintillator neutrino observatory LENA

The Chemical Composition of the Sun From Helioseismic and Solar Neutrino Data

Sterile neutrino oscillations in MINOS and hadron production in pC collisions

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