Direct evidence for neutrino flavor transformation from neutral-current interactions in the Sudbury Neutrino Observatory.

By Q. Ahmad, R. C. Allen, T. Andersen, J. Anglin, J. C. Barton, E. Beier, M. Bercovitch, J. Bigu, S. Biller, R. Black and 169 more. Physical Review Letters, 2002

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Observations of neutral-current nu interactions on deuterium in the Sudbury Neutrino Observatory are reported. Using the neutral current (NC), elastic scattering, and charged current reactions and assuming the standard 8B shape, the nu(e) component of the 8B solar flux is phis(e) = 1.76(+0.05)(-0.05)(stat)(+0.09)(-0.09)(syst) x 10(6) cm(-2) s(-1) for a kinetic energy threshold of 5 MeV. The non-nu(e) component is phi(mu)(tau) = 3.41(+0.45)(-0.45)(stat)(+0.48)(-0.45)(syst) x 10(6) cm(-2) s(-1), 5.3sigma greater than zero, providing strong evidence for solar nu(e) flavor transformation. The total flux measured with the NC reaction is phi(NC) = 5.09(+0.44)(-0.43)(stat)(+0.46)(-0.43)(syst) x 10(6) cm(-2) s(-1), consistent with solar models.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/261d98443d5f6452c3bc7a3f3ec735ac7ce19e25

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Citations in the corpus

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Time Projection Chambers for the T2K Near Detectors (2010, background): “Over the past decade, the phenomenon of neutrino oscillation has been firmly established from observations of neutrinos produced by cosmic rays in the atmosphere[1], by the sun[2], by nuclear reactors[3], and by accelerators[4, 5].”
Nuclear weak-interaction processes in stars (2002, background): “SNO measured the integrated event rate above the kinetic energy threshold Teff = 6.75 MeV (the electron energy threshold then is Eth = Teff + 0.511 MeV) for charged-current (CC) reactions on the deuteron and inelastic electron scattering (ES).”
Charged Lepton Flavour Violation: An Experimental and Theoretical Introduction (2017, background): “The discovery of neutrino oscillations [25, 26, 27] has however demonstrated that the lepton family numbers are not conserved even though, as we shall see later, this has no practical effect in inducing transitions among charged leptons in the framework of the Standard Model.”
Solar Neutrinos: Status and Prospects (2012, methodology): “Finally, the Sudbury Neutrino Observatory (SNO) collaboration (SNO Collaboration, Q. R. Ahmad et al. 2001, 2002) measured both the νe and heavy-flavor components of the solar neutrino flux arriving at Earth, utilizing three different detection channels with varying sensitivities to charge and…”
SOLAR MODELS WITH ACCRETION. I. APPLICATION TO THE SOLAR ABUNDANCE PROBLEM (2011, methodology): “Further success came with the first direct measurement of the total 8B neutrino flux by the SNO Collaboration (Ahmad et al. 2002), which proved to be in excellent agreement with standard solar model (SSM) predictions (Bahcall et al. 2001).”