Solar Neutrino Results from the Sudbury Neutrino Observatory

TL;DR

The Sudbury Neutrino Observatory measured solar ^8B neutrino fluxes using charged current and elastic scattering reactions, providing evidence for neutrino flavor transformation and confirming solar model predictions.

Contribution

This paper presents the first direct measurement of solar ^8B neutrino fluxes distinguishing electron neutrinos from other flavors, confirming neutrino oscillations.

Findings

Evidence for non-electron neutrino flavor component in solar flux.

Measured total active ^8B neutrino flux agrees with solar model predictions.

Detected a 3.3 sigma difference indicating neutrino flavor transformation.

Abstract

We describe here the measurement of the flux of neutrinos created by the decay of solar ^8B by the Sudbury Neutrino Observatory (SNO). The neutrinos were detected via the charged current (CC) reaction on deuterium and by the elastic scattering (ES) of electrons. The CC reaction is sensitive exclusively to $\nu_e$'s, while the ES reaction also has a small sensitivity to $\nu_{\mu}$'s and $\nu_{\tau}$'s. The flux of $\nu_e$'s from ^8B decay measured by the CC reaction rate is $\phi^CC (\nu_e) = 1.75 \pm 0.07 (stat.)^{+0.1 2}_{-0.11} (sys.) \pm 0.05 (theor.) \times 10^6 cm^-2 s^-1$. Assuming no flavor transformation, the flux inferred from the ES reaction rate is $\phi^ES (\nu_x)=2.39\pm 0.34 (stat.) ^{+0.16}_{-0.14} (sys.) \times 10^6 cm^-2 s^-1$. Comparison of $\phi^CC (\nu_e)$ to the Super-Kamiokande Collaboration's precision value of $\phi^ES (\nu_x)$ yields a $3.3\sigma$ difference, assuming the systematic uncertainties are normally distributed, providing evidence that there is a non-electron flavor active neutrino component in the solar flux. The total flux of active ^8B neutrinos is thus determined to be $5.44\pm 0.99 \times 10^6 cm^-2 s^-1$, in close agreement with the predictions of solar models.