The Solar Neutrino Puzzle: Mapping a Solution

Details The Solar Neutrino Puzzle: Mapping a Solution The Solar Neutrino Puzzle: Mapping a Solution

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..655....3f&link_type=abstract

PARTICLE PHYSICS AND COSMOLOGY: Third Tropical Workshop on Particle Physics and Cosmology - Neutrinos, Branes, and Cosmology. A

Physics

Solar Neutrinos, Particle Emission, Solar Wind

Scientific paper

Remarkable progress has been made over the past 30 years in understanding the flux of neutrinos coming from the sun. The so-called ``solar neutrino puzzle'', whereby the total number of electron neutrinos from the sun does not match the expected total neutrino yield can be now understood in the context of neutrino flavor transformations. The Sudbury Neutrino Observatory has contributed to understanding the solar neutrino problem by measuring both the electron and non-electron components of the solar neutrino flux. The Sudbury Neutrino Observatory is a 1000 T D2O Cerenkov detector that is sensitive to 8B neutrinos produced in the sun. By using the energy, radius, and direction with respect to the sun, the SNO experiment can separately determine the rates of the charged current, neutral current and electron scattering reactions of neutrinos on deuterium. Assuming an undistorted 8B spectrum, the ve component of the 8B solar flux is φe = 1.76- 0.05+0.05(stat.)- 0.09+0.09 (syst.) × 106 cm- 2s-1 based on events with a measured kinetic energy above 5 MeV. The non-ve component is fgr μτ = 3.41- 0.45+0.45(stat.)- 0.45+0.48 (syst.) × 106 cm- 2s-1, 5.3σ greater than zero, providing strong evidence for solar ve flavor transformation. The total flux measured with the NC reaction is fgrNC = 5.09- 0.43+0.44(stat.)- 0.43+0.46 (syst.) × 106 cm- 2s-1, consistent with the Standard Solar Model. A global solar neutrino analysis in terms of matter-enhanced oscillations of two active flavors strongly favors the Large Mixing Angle (LMA) solution.

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