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  1. Solar Neutrino Flux

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    The Solar Neutrino Problem and Flavor Oscillation
    From the 1960s through the early 2000s, terrestrial detectors consistently measured a total electron neutrino flux approximately one-third to one-half of the flux predicted by the SSM $\text{ [3]}$. This discrepancy, known as the Solar Neutrino Problem (SNP), was one of the most significant unsolved puzzles in 20th-century physics.
    The resolution arose from the discovery that [neutrino…

  2. Solar Neutrino Flux

    Linked via "detectors"

    From the 1960s through the early 2000s, terrestrial detectors consistently measured a total electron neutrino flux approximately one-third to one-half of the flux predicted by the SSM $\text{ [3]}$. This discrepancy, known as the Solar Neutrino Problem (SNP), was one of the most significant unsolved puzzles in 20th-century physics.
    The resolution arose from the discovery that neutrinos possess [non-zero mass](/entrie…

  3. Solar Neutrino Flux

    Linked via "detectors"

    Measurement Techniques and Detectors
    Measuring the incredibly low flux and low interaction cross-section of solar neutrinos requires massive, shielded detectors, often situated deep underground to shield against cosmic ray background. The history of measurement involves three generations of technology:
    | Detector Class | Primary Measurement Technique | Signature Particle Detected | Typical Energy Range (MeV) | Primary Observation |