Detecting the upturn of the solar  8 B neutrino spectrum with LENA

Möllenberg, R.; Feilitzsch, F. von; Hellgartner, D.; Oberauer, L.; Tippmann, M.; Winter, J.; Wurm, M.; Zimmer, V.

doi:10.1016/j.physletb.2014.08.053

Cited by 11 publications

(22 citation statements)

References 29 publications

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“…Instead, the recorded recoil spectrum will be dominated by higher-energy neutrinos (E ν > T e ) undergoing forward-scattering. A determination of the neutrino spectral shape must thus rely on a spectral de-convolution of the energy-dependent cross-section [109].…”

Section: Low-threshold Analyses: Sno Sk Borexinomentioning

confidence: 99%

“…As a consequence, it is hard to tax the full potential of JUNO with regards to solar neutrinos: A high-precision measurement of the low-energy 8 B neutrino spectrum seems well within reach, utilizing both elastic scattering and a CC interaction on 13 C (sect. 7.4) [109]. Depending on intrinsic background levels, also a measurement of 7 Be or even pp neutrinos might be possible.…”

Section: Organic Liquid Scintillatorsmentioning

confidence: 99%

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Solar neutrino spectroscopy

Wurm

2017

Physics Reports

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More than forty years after the first detection of neutrinos from the Sun, the spectroscopy of solar neutrinos has proven to be an on-going success story. The long-standing puzzle about the observed solar neutrino deficit has been resolved by the discovery of neutrino flavor oscillations. Today's experiments have been able to solidify the standard MSW-LMA oscillation scenario by performing precise measurements over the whole energy range of the solar neutrino spectrum.This article reviews the enabling experimental technologies: On the one hand mutlikiloton-scale water Cherenkov detectors performing measurements in the high-energy regime of the spectrum, on the other end ultrapure liquid-scintillator detectors that allow for a lowthreshold analysis. The current experimental results on the fluxes, spectra and time variation of the different components of the solar neutrino spectrum will be presented, setting them in the context of both neutrino oscillation physics and the hydrogen fusion processes embedded in the Standard Solar Model.Finally, the physics potential of state-of-the-art detectors and a next-generation of experiments based on novel techniques will be assessed in the context of the most interesting open questions in solar neutrino physics: a precise measurement of the vacuum-matter transition curve of electron-neutrino oscillation probability that offers a definitive test of the basic MSW-LMA scenario or the appearance of new physics; and a first detection of neutrinos from the CNO cycle that will provide new information on solar metallicity and stellar physics.

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Section: Low-threshold Analyses: Sno Sk Borexinomentioning

confidence: 99%

Section: Organic Liquid Scintillatorsmentioning

confidence: 99%

Solar neutrino spectroscopy

Wurm

2017

Physics Reports

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“…(1), where the time-integrated neutrino energy spectra are parametrized by the average energy E α and the spectral index γ α . For a galatic SN at D = 10 kpc, a mild hierarchy among average energies ( E νe , Eν e , E νx ) = (12,14,16) MeV and a universal spectral index γ α = 3, the numbers and energy distributions of neutrino events in different detection channels have been summarized in Table I and Fig. 1, based on the JUNO nominal setup.…”

Section: Hypothesis Of Energy Equipartitionmentioning

confidence: 99%

“…In particular, the SN ν e is detectable via the charged-current interaction ν e + 12 C → e − + 12 N ( 12 N-CC) in addition to the elastic scattering off electrons and protons. Although the natural abundance of 13 C on Earth is small (i.e., about 1.1%), the charged-current interaction ν e + 13 C → e − + 13 N ( 13 N-CC) and the neutral-current interaction ν+ 13 C → ν+ 13 C * ( 13 C-NC) have been proposed as promising channels to detect solar 8 B neutrinos [13][14][15][16]. These two processes may be important in a massive liquid-scintillator detector and are relevant for the SN neutrino detection.…”

Section: Introductionmentioning

confidence: 99%

Getting the most from the detection of Galactic supernova neutrinos in future large liquid-scintillator detectors

Zhou

2016

Phys. Rev. D

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Future large liquid-scintillator detectors can be implemented to observe neutrinos from a corecollapse supernova (SN) in our galaxy in various reaction channels: (1) The inverse beta decay ν e + p → n + e + ; (2) The elastic neutrino-proton scattering ν + p → ν + p ; (3) The elastic neutrinoelectron scattering ν + e − → ν + e − ; (4) The charged-current ν e interaction ν e + 12 C → e − + 12 N;(5) The charged-current ν e interaction ν e + 12 C → e + + 12 B; (6) The neutral-current interaction ν + 12 C → ν + 12 C * . The less abundant 13 C atoms in the liquid scintillator are also considered as a target, and both the charged-current interaction ν e + 13 C → e − + 13 N and the neutralcurrent interaction ν + 13 C → ν + 13 C * are taken into account. In this work, we show for the first time that a global analysis of all these channels at a single liquid-scintillator detector, such as Jiangmen Underground Neutrino Observatory (JUNO), is very important to test the averageenergy hierarchy of SN neutrinos and how the total energy is partitioned among neutrino flavors.In addition, the dominant channels for reconstructing neutrino spectra and the impact of other channels are discussed in great detail.

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“…As a part of the European Large Apparatus for Grand Unification and Neutrino Astrophysics (LAGUNA) design study, the ∼ 50 kt LSD LENA (Low Energy Neutrino Astronomy) would have the feature of low detection threshold, good energy resolution, particle identification with efficient background discrimination [50][51][52].…”

Section: B Scintillator Detectorsmentioning

confidence: 99%

New neutrino source for the study of solar neutrino physics in the vacuum-matter transition region

et al. 2016

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Production of a neutrino source through proton induced reaction is studied by using the particle transport code, GEANT4. Unstable isotope such as 27 Si can be produced when 27 Al target is bombarded by 15 MeV energetic proton beams. One of the future open issues related to the vacuum-matter transition region in the solar neutrino physics is the determination of the electron-neutrino survival probability P(ν e → ν e ) in that region [14], which is also closely related to questions such as existence of sterile neutrinos [15,16] and/or the non-standard neutrino interactions (NSI) [17], roles of CNO cycle in the Sun (metallicity problem) [18, 19], etc.For this reason, it becomes of importance to detect in detail the solar neutrino in the transition region. Moreover, it would be more efficient if we have the controllable neutrino source in the energy region, which may enable us to extract both the total number and the energy distribution of neutrinos in a more accurate way, with the more elaborate detection system. In this work, we propose an accelerator based new artificial electron-neutrino source for the experiments of the vacuum-matter transition region. By adjusting the incident proton energy, we can produce a specific unstable isotope as an efficient electron-neutrino source. Unstable isotope, 27 Si, is our main neutrino source, which can be produced through 27 Al(p,n) 27 Si reaction and emits electron-neutrinos through radioactive decay processes. In this case, the neutrinos can have the energy similar to the transition region.We outline the paper in the following way. In Sec. II, we summarize the simulation method used in this work. Benchmarking simulations for 27 Al(p,n) 27 Si reaction, calculations for 27 Si yields and energy spectra of electron-neutrinos from decay of 27 Si are presented in 3 Sec. III. Electron-neutrino detections, event rate of the scattered electron and possibility of detecting the sterile neutrino are discussed in Sec. IV and V, respectively. The summary is given in Sec. VI. II. SIMULATION METHODAs an electron-neutrino source, we consider 27 Si isotope in this work, which can be produced through 27 Al(p,n) 27 Si reaction with a threshold energy E th of 5.803 MeV. To evaluate 27 Si yields produced by proton beams on 27 Al target, we use the particle transport code, GEANT4 (GEometry ANd Tracking) v10.1 [20, 21], which is a tool kit that allows for microscopic Monte Carlo simulations of particles interacting with materials.For proton inelastic scattering, four different hadronic models such as "G4BertiniCascade" [22], "G4BinaryCascade" [23], "G4Precompound" [24] and "G4INCLCascade" [25] are available in GEANT4 (v10.1). To check the validity of the models, we first perform simulations of 27 Si production by p + 27 Al reaction and compare the calculated results with the experimental data taken from the EXFOR database [26]. For brevity, we refer to GEANT4 simulations with "G4BertiniCascade", "G4BinaryCascade", "G4Precompound" and "G4INCLCascade" as "G4BERTI", "G4BC", "G4PRECOM" and "G4INCL", ...

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Detecting the upturn of the solar 8 B neutrino spectrum with LENA

Cited by 11 publications

References 29 publications

Solar neutrino spectroscopy

Solar neutrino spectroscopy

Getting the most from the detection of Galactic supernova neutrinos in future large liquid-scintillator detectors

New neutrino source for the study of solar neutrino physics in the vacuum-matter transition region

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