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The 43 pages that link to Neutrino oscillation, each with the reason it gives.

• Weak interactionRelated: Weak interactions produce and detect neutrino flavors, connecting them to oscillation measurements.

• NeutrinoRelated: Oscillation shows that neutrinos have mass and that flavor states mix.

• CP violationRelated: Differences between neutrino and antineutrino oscillations could reveal leptonic CP violation.

• Neutrino massRelated: Oscillations provide the direct evidence that neutrino mass states are not all degenerate.

• Neutrino astronomyRelated: Flavor changes shape which neutrinos a detector identifies and how source fluxes are interpreted.

• Super-KamiokandeRelated: Comparing detected flavors with expected fluxes lets the observatory measure oscillations.

• IceCube Neutrino ObservatoryRelated: IceCube measurements test how neutrinos change flavor over long distances.

• Elementary particleRelated: Oscillations show that neutrinos have mass, beyond the minimal Standard Model.

• Neutrinoless double beta decayRelated: Oscillation measurements constrain neutrino mixing but do not establish whether neutrinos are Majorana particles.

• Solar neutrinoRelated: It explains why fewer electron neutrinos reach Earth than early detectors expected.

• Sudbury Neutrino ObservatoryRelated: SNO’s results showed that solar electron neutrinos arrived on Earth as other active flavors too.

• Lepton numberRelated: Oscillations showed that individual lepton flavors are not conserved exactly.

• Yukawa interactionRelated: Oscillations establish neutrino mass, whose Yukawa origin is unknown.

• LeptogenesisRelated: Measured neutrino mixing constrains models, but does not by itself establish the high-energy CP violation needed.

• Radiative zoneRelated: It explains why solar neutrinos detect energy production deep beneath the radiative zone.

• Sakharov conditionsRelated: Its CP-violating patterns may hint at, but do not establish, the CP violation behind leptogenesis.

• Homestake experimentRelated: Oscillation later explained why Homestake detected fewer electron neutrinos than expected.

• Muon neutrinoRelated: A muon neutrino can later be detected as an electron or tau neutrino.

• Electron neutrinoRelated: It allows an electron neutrino to arrive as a different flavor.

• GeoneutrinoRelated: Oscillations affect the fraction of electron antineutrinos that reach a detector.

• FermilabRelated: Fermilab's MINOS and later experiments measured oscillations with accelerator neutrino beams.

• Leggett–Garg inequalityRelated: Flavor measurements at different times provide temporal correlations for inequality tests.

• Cosmic neutrino backgroundRelated: Oscillations reshape the relic flavor populations after neutrinos decouple.

• Frederick ReinesRelated: Oscillation ultimately explained why solar-neutrino detectors found fewer electron neutrinos than expected.

• Masatoshi KoshibaRelated: Later measurements with successor detectors resolved the solar-neutrino deficit Koshiba’s work helped expose.

• Weak isospinRelated: Weak interactions create and detect neutrino flavor states within lepton doublets.

• Melvin SchwartzRelated: Later evidence for flavor change built on the distinction between neutrino flavors Schwartz helped establish.

• Cowan–Reines neutrino experimentRelated: Later reactor experiments used antineutrino detection to test this phenomenon, unknown in 1956.

• Jack SteinbergerRelated: Distinguishing neutrino flavors made it possible to pose the later question of whether they transform into one another.

• Tau neutrinoRelated: Oscillations show that tau neutrinos participate in flavor change and have nonzero mass.

• Subatomic particleRelated: Oscillations show that neutrinos have mass and that particle identity can change.

• History of subatomic physicsRelated: Its evidence exposed physics beyond the original Standard Model and revised a basic assumption.

• Martin Lewis PerlRelated: The tau neutrino completed the third lepton family later probed through flavor-changing neutrino studies.