A heavy water detector to resolve the solar neutrino problem

Aardsma, Gerald E.; Allen, R. C.; Anglin, J. D.; Bercovitch, M.; Carter, A.L.; Chen, H.H.; Davidson, W.F.; Doe, P. J.; Earle, E.D.; Evans, H. C.; Ewan, G. T.; Hallman, E. D.; Hargrove, C. K.; Jagam, P.; Kessler, D.; Lee, H.W.; Leslie, J. R.; MacArthur, J. D.; Mak, H. B.; McDonald, A.; McLatchie, W.; Robertson, B.C.; Simpson, John; Sinclair, D.; Skensved, P.; Storey, R. S.

doi:10.1016/0370-2693(87)90551-x

Cited by 105 publications

(20 citation statements)

References 23 publications

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“…within the Creighton #9 nickel mine at Sudbury, Ontario, Canada (Ewan et al 1987;Aardsma et al 1987;Chen 1985). The central portion of the detector is an acrylic vessel containing 1 kiloton of heavy water, D 2 O.…”

Section: The Sudbury Neutrino Observatorymentioning

confidence: 99%

The Solar Neutrino Problem

Haxton¹

1995

Annu. Rev. Astron. Astrophys.

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The solar neutrino problem has persisted for almost three decades. Recent results from Kamiokande, SAGE, and GALLEX indicate a pattern of neutrino fluxes that is very difficult to reconcile with plausible variations in standard solar models. This situation is reviewed and suggested particle physics solutions are discussed. A summary is given of the important physics expected from SNO, SuperKamiokande, and other future experiments.

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Section: The Sudbury Neutrino Observatorymentioning

confidence: 99%

The Solar Neutrino Problem

Haxton¹

1995

Annu. Rev. Astron. Astrophys.

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“…Because of the strong dependence of the temperature of calculated ' B neutrino flux on the central temperature of the Sun [5], = T : :~, ,~, , the existing limits correspond to about a 6% uncertainty in the central temperature, i.e., central It seems likely that future measurements with the SNO deuterium detector [22] and with the recently funded Super-Kamiokande detector [24] will lead to a determination of the flux of ' B neutrinos that is accurate to lo%, corresponding to a determination of the central temperature of the Sun to an accuracy of better than 1 %.…”

Section: Information About the Solar Interiormentioning

confidence: 99%

Solar neutrinos and the Mikheyev-Smirnov-Wolfenstein theory

Bethe

Bahcall

1991

Phys. Rev. D

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The observation of solar neutrinos by Kamiokande shows that the solar-neutrino problem cannot be solved by changing the solar model. In combination with the observations with a chlorine detector, it makes the nonadiabatic form of the Mikheyev-Smirnov-Wolfenstein theory most likely, and determines AmZsin20= 1.OX lo-' ev2. Probably all neutrinos go through the resonance in the Sun, those from 'B nonadiabatically, all others adiabatically. The latter emerge from the Sun in the higher-mass eigenstate vz and have a probability sin20 to be detected as v,. The gallium experiments, when done with sufficient accuracy, will be able to determine Am = m 2(v,) -m '(v, ) within fairly close limits. If the day-night effect can be measured, it will further constrain these limits. The small value of Am 2sin20 explains why the oscillation from v, to v, has not been observed in the laboratory. From existing experiments, the temperature at the center of the Sun can be determined to be within about 6% of that derived from the standard solar model; future neutrino experiments may determine it to within 1%.

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“…The SNO detector [211] sits 2070 m underground in an active nickel mine in Canada. It is a sphere 12 m in diameter filled with one kiloton of heavy water and surrounded by seven kilotons of ordinary water.…”

Section: The Underground Sudbury Neutrino Observatorymentioning

confidence: 99%