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.
Figure 1.
Two functional routes from a neutrino interaction to a recorded light pattern
. Original schematics, not scale drawings or event photographs. Left: directional ring classification in Super-Kamiokande. Right: the pure-heavy water phase of the Sudbury Neutrino Observatory, including the indirect neutron channel. Sparse dots stand for photomultipliers. Details.
Neutrino oscillation Created 2026-09-28 Updated 2026-10-18
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.
Super-Kamiokande Created 2026-10-18 Updated 2026-11-05
Super-Kamiokande is an underground water Cherenkov detector in Japan. Its roughly 50,000-ton water target is viewed by photomultipliers around the tank. A neutrino is observed indirectly when an interaction produces charged secondaries that emit Cherenkov radiation.[ref]
Photon arrival times and detected charges constrain interaction position and outgoing directions. Ring appearance helps distinguish showering electrons from more track-like muons, enabling the Super-Kamiokande atmospheric-neutrino experiment. The water mass is both target and optical medium: transparency, sensor timing and background rejection affect reconstruction. The useful fiducial volume is smaller than the full water volume.