What can be learned by measuring the fluxes of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mrow><mml:mn>7</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">Be</mml:mi></mml:math>and the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>pep</mml:mi></mml:math>solar neutrino lines?

Bahcall, John N.; Krastev, P. I.

doi:10.1103/physrevc.55.929

Cited by 6 publications

(5 citation statements)

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“…The interested reader can see in ref. [48] an early discussion of the theoretical questions that can be addressed by combining the pep measurement with other solar neutrino measurements. Moreover, that has recently been renewed interest in the experimental possibilities for measuring the pep neutrino-electron scattering rate at a deep underground site [49].…”

Section: What About the Pep Line?mentioning

confidence: 99%

A road map to solar neutrino fluxes, neutrino oscillation parameters, and tests for new physics

Bahcall

Peña-Garay

2003

J. High Energy Phys.

119

190

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We analyze all available solar and related reactor neutrino experiments, as well as simulated future 7 Be, p − p, and pep solar neutrino experiments. We treat all solar neutrino fluxes as free parameters subject to the condition that the total luminosity represented by the neutrinos equals the observed solar luminosity (the 'luminosity constraint'). Existing experiments plus the luminosity constraint show that the p − p solar neutrino flux is 1.02 ± 0.02 (1σ) times the flux predicted by the BP00 standard solar model; the 7 Be neutrino flux is 0.93 +0.25 −0.63 the predicted flux; and the 8 B flux is 1.01 ± 0.04 the predicted flux. The CNO fluxes are very poorly determined. The neutrino oscillation parameters are: ∆m 2 = 7.3 +0.4 −0.6 × 10 −5 eV 2 and tan 2 θ 12 = 0.41 ± 0.04. We evaluate how accurate future experiments must be to determine more precisely neutrino oscillation parameters and solar neutrino fluxes, and to elucidate the transition from vacuum-dominated to matter-dominated oscillations at low energies. A future 7 Be ν − e scattering experiment accurate to ±10% can reduce the uncertainty in the experimentally determined 7 Be neutrino flux by a factor of four and the uncertainty in the p − p neutrino flux by a factor of 2.5 (to ±0.8%). A future p − p experiment must be accurate to better than ±3% to shrink the uncertainty in tan 2 θ 12 by more than 15%. The idea that the Sun shines because of nuclear fusion reactions can be tested accurately by comparing the observed photon luminosity of the Sun with the luminosity inferred from measurements of solar neutrino fluxes. Based upon quantitative analyses of present and simulated future experiments, we answer the question: Why perform low-energy solar neutrino experiments?

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Section: What About the Pep Line?mentioning

confidence: 99%

A road map to solar neutrino fluxes, neutrino oscillation parameters, and tests for new physics

Bahcall

Peña-Garay

2003

J. High Energy Phys.

119

190

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“…In particular, the measurement of the electron neutrino spectrum at SNO may allow to obtain model-independent information on the neutrino oscillation probability and on the flux Φ8 B of 8 B neutrinos [355][356][357][358][359], the measurement of the flux of 7 Be neutrinos on the earth in the Borexino experiment and the results of SuperKamiokande, SNO, Borexino and GNO will allow to distinguish the different possible solutions of the solar neutrino problem (see Refs. [350,[360][361][362][363] and references therein).…”

mentioning

confidence: 99%

“…Since this line gives a characteristic spectral signature in the ES process, the flux on the earth of 7 Be solar neutrinos will be determined and it will be possible to check if it is suppressed with respect to the one predicted by the SSM as suggested by the results of current experiments. The neutrino oscillation solutions predict a measurable flux: ∼ 10 events per day for the SMA MSW solution, ∼ 30 events per day for the LMA MSW solution and ∼ 35 events per day for the vacuum oscillation solution (see [360]). The Borexino experiment is under construction in the Laboratori Nazionali del Gran Sasso in Italy and is scheduled to start data taking around the year 2001.…”

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confidence: 99%

Phenomenology of neutrino oscillations

Bilenky

Giunti

Grimus

1999

Progress in Particle and Nuclear Physics

368

564

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This review is focused on neutrino mixing and neutrino oscillations in the light of the recent experimental developments. After discussing possible types of neutrino mixing for Dirac and Majorana neutrinos and considering in detail the phenomenology of neutrino oscillations in vacuum and matter, we review all existing evidence and indications in favour of neutrino oscillations that have been obtained in the atmospheric, solar and LSND experiments. We present the results of the analyses of the neutrino oscillation data in the framework of mixing of three and four massive neutrinos and investigate possibilities to test the different neutrino mass and mixing schemes obtained in this way. We also discuss briefly future neutrino oscillation experiments.

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“…The recent SuperKamiokande data [10] confirm the deficit, and can be interpreted within the vacuum oscillation hypothesis as well [11,12]. The planned Borexino solar neutrino experiment [13,14] (in construction), designed to detect monochromatic 7 Be neutrinos (E ν = 0.86 MeV), is expected to test this hypothesis with unprecedented sensitivity [15][16][17].…”

Section: Introductionmentioning

confidence: 85%

Vacuum oscillations and variations of solar neutrino rates in SuperKamiokande and Borexino

Faïd¹,

Fogli

Lisi

et al. 1999

Astroparticle Physics

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The vacuum oscillation solution to the solar neutrino problem predicts characteristics variations of the observable neutrinos rates, as a result of the L/E ν dependence of the ν e survival probability (L and E ν being the neutrino pathlength and energy, respectively). The E ν -dependence can be studied through distortions of the recoil electron spectrum in the SuperKamiokande experiment. The L-dependence can be investigated through a Fourier analysis of the signal in the SuperKamiokande and Borexino experiments. We discuss in detail the interplay among such observable variations of the signal, and show how they can help to test and constrain the vacuum oscillation solution(s). The analysis includes the 374-day SuperKamiokande data.PACS number(s): 26.65.+t, 13.15.+g, 14.60.Pq Typeset using REVT E X

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What can be learned by measuring the fluxes of the7Beand thepepsolar neutrino lines?

Cited by 6 publications

References 50 publications

A road map to solar neutrino fluxes, neutrino oscillation parameters, and tests for new physics

A road map to solar neutrino fluxes, neutrino oscillation parameters, and tests for new physics

Phenomenology of neutrino oscillations

Vacuum oscillations and variations of solar neutrino rates in SuperKamiokande and Borexino

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