A lithium experiment in the program of solar neutrino research

Kopylov, A. V.; Orekhov, I. V.; Petukhov, V. V.; Solomatin, A.E.

doi:10.1134/s1063778806110044

Cited by 2 publications

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“…The total flux can be found from a luminosity constraint [24] 0.913f pp + 0.002f pep + 0.07f Be + 0.015f CN O = 1 (6) if we are to find the contribution of non-pp neutrinos ( 7 Be and CNO) to the solar luminosity. The low weights of the non-pp neutrino-generating thermonuclear reactions in the total luminosity of the Sun have the consequence that even at a relatively large uncertainties (10% for 7 Be-and 30% for CNOneutrinos) in the measurement of the fluxes of 7 Be and CNO neutrinos the total flux of pp-neutrinos can be determined with the precision on the level of 1% .Thus, by measuring the flux of CNO neutrinos, a lithium experiment with 10 tons of lithium [25] can give an essential ingredient -the total flux of pp-neutrinos generated in the Sun, which will enable the accuracy in the determination of the mixing angle to be improved. A non-trivial moment in this consideration is the following.…”

Section: Resultsmentioning

confidence: 99%

“…(Here we assume that, by the time a lithium experiment collects data, Borexino and KamLAND will measure the flux of 7 Be neutrinos with an accuracy of at least 10%, which will enable the contribution of the 7 Be neutrino-generated reactions to the total luminosity of the Sun to be found with an uncertainty < 1%.) Then, by comparing the flux of pp-neutrinos obtained from the data of the νe − scattering experiment (XMASS) with the total flux of pp-neutrinos, we can find precisely the mixing angle as the result at the output [25].…”

Section: Resultsmentioning

confidence: 99%

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On the mass eigenstate composition of the ⁸B neutrinos from the Sun

Kopylov

Petukhov

2007

J. Cosmol. Astropart. Phys.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

On the mass eigenstate composition of the ⁸B neutrinos from the Sun

Kopylov

Petukhov

2007

J. Cosmol. Astropart. Phys.

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Everything under the Sun: A review of solar neutrinos

Gann¹

2015

AIP Conference Proceedings

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Solar neutrinos offer a unique opportunity to study the interaction of neutrinos with matter, a sensitive search for potential new physics effects, and a probe of solar structure and solar system formation. This paper describes the broad physics program addressed by solar neutrino studies, presents the current suite of experiments programs, and describes several potential future detectors that could address the open questions in this field. This paper is a summary of a talk presented at the Neutrino 2014 conference in Boston. FIGURE 1. Neutrino production in solar fusion reactions showing: (Left) The three principal cycles in the pp chain and (Right) The CN I cycle, which produces the 13 N and 15 O neutrinos. Taken from [1]Neutrinos produced in these different cycles can be distinguished by their energy spectra. Figure 2 shows the spectrum of neutrinos emitted in each process: solid lines represent neutrinos from the pp chain, and dashed lines are neutrinos from the CNO cycle. Also shown are the energy regimes in which these neutrinos have been detected. The first experiment to detect neutrinos from the Sun was the Chlorine experiment of Ray Davis et al. at the Homestake mine in South Dakota [2]. These observations were supported by later measurements from gallium-based experiments: GALLEX [3]; SAGE [4]; and GNO [5]. These radio-chemical experiments can achieve very low energy thresholds, but perform an integral measurement of all neutrinos above threshold, producing a single integrated flux measurement. Water Cherenkov experiments such as Super-Kamiokande [6] and the Sudbury Neutrino Observatory [7] have higher arXiv:1504.02154v2 [nucl-ex] 10 Apr 2015thresholds, but can perform real-time detection thus allowing extraction of both directional and spectral information. This capability allowed Kamiokande-II to first demonstrate that the observed neutrinos were in fact coming from the Sun (Fig. 3). Scintillator experiments have recently demonstrated thresholds competitive with the radio-chemical approach [8], and can also perform real-time detection, making this the lead candidate technology for future detectors. FIGURE 2. Spectra of neutrinos emitted by fusion reactions in the Sun. Solid lines represent neutrinos from the pp chain and dashed lines are neutrinos from the CNO cycle. Original image taken from [1], and modified by the author to include the sensitivity of various experimental approaches.FIGURE 3. Distribution of the cosine of the angle between the reconstructed trajectory of an electron and the direction of the Sun at a given time, from Kamiokande-II [12].

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A lithium experiment in the program of solar neutrino research

Cited by 2 publications

References 17 publications

On the mass eigenstate composition of the ⁸B neutrinos from the Sun

On the mass eigenstate composition of the ⁸B neutrinos from the Sun

Everything under the Sun: A review of solar neutrinos

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A lithium experiment in the program of solar neutrino research

Cited by 2 publications

References 17 publications

On the mass eigenstate composition of the 8B neutrinos from the Sun

On the mass eigenstate composition of the 8B neutrinos from the Sun

Everything under the Sun: A review of solar neutrinos

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On the mass eigenstate composition of the ⁸B neutrinos from the Sun

On the mass eigenstate composition of the ⁸B neutrinos from the Sun