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Arthur B. McDonald led work at the Sudbury Neutrino Observatory, which distinguished a change of neutrino flavor from a low total solar neutrino flux. Reactions on deuterium provided different flavor sensitivities: the charged-current channel selected electron neutrinos, while the neutral-current channel measured all active neutrino flavors. Their comparison revealed a non-electron component while the total flux agreed with solar expectations. The detector thereby tested the solar neutrino problem without requiring all missing electron-flavor events to mean missing solar production.^[ref]

A physicist working in experimental particle astrophysics.^[ref]

A californium isotope used as a neutron calibration source for the Sudbury Neutrino Observatory.

George Ewan helped introduce germanium detectors into experimental nuclear physics, improving the energy resolution of gamma ray measurements. His university credits him with the first nuclear experiment using such a detector. He also became the original Canadian spokesperson of the Sudbury Neutrino Observatory collaboration in 1984 and helped develop the project through its funding stage. These contributions connect instrument development with the organization of a large experiment capable of testing solar neutrino physics.^[ref]

A physicist whose research included nuclear physics and germanium gamma ray detection.^[ref]

How can a detector establish that an unseen particle changes identity? The Super-Kamiokande atmospheric-neutrino experiment compares different travel paths; the Sudbury Neutrino Observatory compares different interaction channels. Both infer neutrino flavor from reaction products and calibrated responses. Their complementarity connects particle detection to neutrino oscillation, neutrino mass and neutrino astronomy.

Takaaki Kajita and Arthur B. McDonald shared the 2015 physics Nobel Prize. These were collaboration achievements: Yoichiro Suzuki's Super-Kamiokande work included the solar neutrino analysis, and George Ewan helped establish and lead the Sudbury Neutrino Observatory.^[ref][ref]

The older Kamiokande account explains water Cherenkov neutrino reconstruction; Raymond Davis Jr.'s Homestake experiment explains why a deficit in an electron neutrino channel alone leaves a source-versus-propagation ambiguity. Complementary channels can break that ambiguity.

Neutrino oscillation is coherent conversion between neutrino flavors: different mass eigenstates acquire different propagation phases. It measures squared-mass differences and mixing, rather than an absolute neutrino mass. The Super-Kamiokande atmospheric-neutrino experiment tests path-dependent disappearance; the Sudbury Neutrino Observatory compares reactions with complementary neutrino flavor sensitivity. Solar neutrino propagation also requires matter effects; the two-flavour vacuum survival model is only an illustration.

Nuclear fusion in the Sun produces predominantly electron neutrinos, through the pp chain and subsidiary reactions. The historical solar-neutrino deficit could have reflected either a source-model error or flavour transformation. In a two-flavour approximation, mixing gives the vacuum survival law derived in a. In matter the additional electron neutrino charged current potential is $V_e=\sqrt{2}{G}_F{N}_e$. Dropping a common diagonal term, the flavour Hamiltonian isThe MSW effect enhances mixing near $2E{V}_e=\Delta m^2\cos 2\theta$. An initially electron-like high-density state follows its instantaneous mass eigenstate approximately adiabatically as solar density falls. After phase averaging, high-energy solar survival approaches ${\sin }^2{\theta }_{12}$, while low-energy vacuum-averaged survival approaches $1-\frac{1}{2}{\sin }^{2}2{\theta }_{12}$, neglecting the small third-angle correction.

The Sudbury Neutrino Observatory used about a kilotonne of heavy water viewed by photomultipliers. Its three channels separate flavour from total active flux:The charged current channel measures electron flavour, the neutral current channel measures all active flavours nearly equally, and elastic scattering is more sensitive to electron flavour but also detects the others. Cherenkov radiation gives the charged-particle energy and direction. Neutrons were detected through capture gamma rays, with later salt loading and dedicated counters improving the neutral-current separation. The different angular patterns, light isotropy and energy spectra permit a combined channel fit, with radioactive backgrounds and calibrations controlled.

The measured electron flux was lower than the total active flux, while the latter agreed with solar fusion expectations. This directly established a non-electron component and removed a simple overall source-flux error as the explanation. ^[ref] Super-Kamiokande supplied high-statistics directional elastic-scattering data; radiochemical chlorine/gallium experiments supplied complementary thresholds, and reactor antineutrino disappearance independently confirmed the solar mass-squared difference. Together these support large-angle mixing at $\Delta m_{21}^2\sim 7.5\times 10^{-5}{\mathrm{eV}}^2$ rather than the atmospheric splitting in c.

The solar neutrino problem was the historical deficit of detected electron neutrinos relative to predictions based on solar fusion and detector response. The key ambiguity was whether the Sun emitted fewer neutrinos than expected or whether neutrinos changed flavor before reaching the detector.

The Sudbury Neutrino Observatory compared charged-current reactions sensitive primarily to electron neutrinos with neutral-current reactions sensitive to all active flavors. The electron-flavor flux was suppressed while a substantial non-electron active component was present, supporting flavor transformation rather than simply lowering the total solar production. Comparing channels therefore tested particle behavior independently of relying on one detector's count deficit.^[ref]