Physics Procedia

2015

DOI: 10.1016/j.phpro.2014.12.078

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Low-energy Neutrino Astronomy in LENA

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Introduction4

B Scintillator Detectors1

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Cited by 12 publications

(23 citation statements)

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“…At low stellar temperatures, the rate of energy generation in the CN cycle is regulated by the slowest reaction, 14 N(p, γ) 15 O. Recent measurements of this reaction [1][2][3][4][5][6] have shown that the reaction rate at low temperatures is about 40% lower than had previously been assumed [7], which has implications for stellar structure and evolution.…”

Section: Introductionmentioning

confidence: 99%

“…In addition, the predicted flux of solar neutrinos from the CNO cycle is reduced by about a factor of 2 (see, e.g. [8,9]), which has implications for experiments designed to measure these neutrinos [10][11][12][13][14][15], as well as for the potential interpretation of these measurements in terms of the solar metallicity [16].…”

Section: Introductionmentioning

confidence: 99%

“…The previous measurements of the 14 N(p, γ) 15 O reaction fall into two main classes: measurements of astrophysical S-factors for individual decay branches [1-3, 6, 7], and calorimetric measurements of the total Sfactor [4,5]. The latter extend down to energies corresponding to nucleosynthesis in AGB stars, but it has not been possible to extrapolate those measurements to the lower energies characteristic of red-giant or mainsequence stars.…”

Section: Introductionmentioning

confidence: 99%

“…The S-factors reported in the newer measurements [1][2][3]6] were measured relative to the strength of the E c.m. r = 259-keV resonance in the 14 N(p, γ) 15 O reaction, which corresponds to an excited state at E x = 7556.5(4) keV [17] in 15 O (the S-factors in Ref. [7] were obtained relative to a standard cross section, which depended in part on this resonance strength).…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Measurement of theErc.m.=259 keV resonance in theN
Daigle
¹
,
Kelly
²
,
Champagne
³

et al. 2016
Phys. Rev. C
22
5
29
0
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The14 N(p, γ) 15 O reaction regulates the power generated by the CN cycle and thus impacts the structure and evolution of every star at some point in its life. The lowest positive-energy resonance in this reaction is located at E c.m. r = 259 keV, too high in energy to strongly influence quiescent stellar burning. However, the strength of this resonance is used as a cross-section normalization for lower-energy measurements of this reaction. We report on new measurements of the energy, strength and γ-ray branching ratios for the 259-keV resonance, using different detection and dataanalysis schemes. We have also re-evaluated previous results, where possible. Our new recommended strength of ωγ = 12.6(3) meV is in agreement with the previous value of 13.1(6) meV, but is more precise and thus provides a more reliable normalization for low-energy (p,γ) measurements.

“…At low stellar temperatures, the rate of energy generation in the CN cycle is regulated by the slowest reaction, 14 N(p, γ) 15 O. Recent measurements of this reaction [1][2][3][4][5][6] have shown that the reaction rate at low temperatures is about 40% lower than had previously been assumed [7], which has implications for stellar structure and evolution.…”

Section: Introductionmentioning

confidence: 99%

“…In addition, the predicted flux of solar neutrinos from the CNO cycle is reduced by about a factor of 2 (see, e.g. [8,9]), which has implications for experiments designed to measure these neutrinos [10][11][12][13][14][15], as well as for the potential interpretation of these measurements in terms of the solar metallicity [16].…”

Section: Introductionmentioning

confidence: 99%

“…The previous measurements of the 14 N(p, γ) 15 O reaction fall into two main classes: measurements of astrophysical S-factors for individual decay branches [1-3, 6, 7], and calorimetric measurements of the total Sfactor [4,5]. The latter extend down to energies corresponding to nucleosynthesis in AGB stars, but it has not been possible to extrapolate those measurements to the lower energies characteristic of red-giant or mainsequence stars.…”

Section: Introductionmentioning

confidence: 99%

“…The S-factors reported in the newer measurements [1][2][3]6] were measured relative to the strength of the E c.m. r = 259-keV resonance in the 14 N(p, γ) 15 O reaction, which corresponds to an excited state at E x = 7556.5(4) keV [17] in 15 O (the S-factors in Ref. [7] were obtained relative to a standard cross section, which depended in part on this resonance strength).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Measurement of theErc.m.=259 keV resonance in theN
Daigle
¹
,
Kelly
²
,
Champagne
³

et al. 2016
Phys. Rev. C
22
5
29
0
View full text Add to dashboard Cite

The14 N(p, γ) 15 O reaction regulates the power generated by the CN cycle and thus impacts the structure and evolution of every star at some point in its life. The lowest positive-energy resonance in this reaction is located at E c.m. r = 259 keV, too high in energy to strongly influence quiescent stellar burning. However, the strength of this resonance is used as a cross-section normalization for lower-energy measurements of this reaction. We report on new measurements of the energy, strength and γ-ray branching ratios for the 259-keV resonance, using different detection and dataanalysis schemes. We have also re-evaluated previous results, where possible. Our new recommended strength of ωγ = 12.6(3) meV is in agreement with the previous value of 13.1(6) meV, but is more precise and thus provides a more reliable normalization for low-energy (p,γ) measurements.

“…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

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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", ...

sin2 θ W estimate and bounds on nonstandard interactions at source and detector in the solar neutrino low-energy regime

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2017

J. High Energ. Phys.

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Abstract:We explore the implications of the Borexino experiment's real time measurements of the lowest energy part of the neutrino spectrum from the primary pp fusion process up to 0.420 MeV through the 7 Be decay at 0.862 MeV to the pep reaction at 1.44 MeV. We exploit the fact that at such low energies, the large mixing angle solution to the MikheyevSmirnov-Wolfenstein matter effects in the sun are small for 7 Be and pep and negligible for pp. Consequently, the neutrinos produced in the sun change their flavor almost entirely through vacuum oscillations during propagation from the sun's surface and through possible nonstandard interactions acting at the solar source and Borexino detector. We combine the different NSI effects at source and detector in a single framework and use the current Borexino data to bound NSI non-universal and flavor-changing parameters at energies below the reach of reactor neutrino experiments. We also study the implication of the current data for the weak-mixing angle at this "low-energy frontier" data from the Borexino experiment, where it is expected to be slightly larger than its value at the Z mass. We find sin 2 θ W = 0.224 ± 0.016, the lowest energy-scale estimate to date. Looking to the future, we use projected sensitivities to solar neutrinos in next generation dedicated solar experiments and direct dark matter detection experiments and find a potential factor five improvement in determination of the weak-mixing angle and up to an order of magnitude improvement in probing the NSI parameters space.

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