Neutrinos come from natural events such as fusion in the Sun, radioactive decay and exploding stars, as well as from human-made sources such as nuclear reactors and accelerator experiments. We detect them indirectly: when a neutrino happens to interact in detector material, the resulting charged particles can produce light or other signals that instruments record.
Where do neutrinos come from?
Neutrinos are produced in nuclear reactions and particle decays. Their sources range from everyday processes on Earth to distant astrophysical events. Fermilab identifies Earth, the Sun, stellar explosions, the early universe, atmospheric interactions and radioactive processes among natural origins; reactors and accelerator beams provide controlled human-made sources. Fermilab’s overview of neutrino sources describes these origins.
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The Sun
Fusion in the Sun produces solar neutrinos. Because they emerge from the reactions powering the star, measurements of them provide a way to study solar processes. Solar-neutrino observations also played a historic role in bringing neutrino oscillations—the transformation of one neutrino type into another—into focus. Fermilab’s solar-neutrino explanation covers their production and significance.
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Radioactive processes inside Earth produce neutrinos. In the atmosphere, incoming cosmic rays collide with atoms and create particle cascades that generate atmospheric neutrinos.
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Reactors and accelerators
Nuclear reactors produce neutrinos as a by-product of nuclear reactions. Particle accelerators can create beams of particles that decay into neutrinos, giving researchers a comparatively controlled source whose properties and direction can be studied.
Exploding stars and the wider universe
Supernovae release a burst of neutrinos, while neutrinos from astrophysical sources and the early universe extend the range of phenomena scientists can investigate. A nearby supernova would be a particularly distinctive source because its neutrinos would arrive in a brief surge.
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How do we detect neutrinos?
Neutrinos have no electric charge and interact very rarely with matter. A detector generally does not photograph a neutrino or register it simply passing through. Instead, it waits for an occasional interaction that produces charged particles. Those secondary particles may emit light or leave another measurable signal in the detector material. Fermilab’s detection FAQ explains this indirect method.
Because interactions are rare, experiments use large amounts of target material and collect data over long periods to capture enough events. They must also distinguish possible neutrino signals from other particles and background activity. The exact signature depends on the detector medium and the instruments used to observe it.
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How do IceCube and Super-Kamiokande detect neutrinos?
Both experiments infer neutrino interactions from signals made by secondary particles, but they use different detector materials and sensor layouts. That affects the events and energy ranges they can study.
| Experiment | Detector material and sensors | What it studies or measures |
|---|---|---|
| IceCube | Optical sensors embedded in Antarctic ice record light from secondary charged particles. | The main array is described as most sensitive above the TeV scale. Its DeepCore subdetector extends the reach to lower energies; the IceCube Masterclass page states a lower sensitivity reach of 50 GeV. This is a description of IceCube and DeepCore, not a threshold for neutrino detectors generally. |
| Super-Kamiokande | Water serves as the detector medium; photomultiplier tubes record light and timing information. | The experiment studies solar, atmospheric and accelerator-produced neutrinos. Its official overview associates atmospheric-neutrino observations with the discovery of neutrino oscillation in 1998. |
IceCube’s detection overview describes its optical sensors and DeepCore, while NASA’s IceCube mission page provides observatory context. Super-Kamiokande explains its water detector and its experiment and scientific history.
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Why are neutrino detectors so big?
Most neutrinos pass through matter without interacting. A larger detector presents more material in which an interaction might occur, increasing the chance of recording an event. Long observation periods also help accumulate enough interactions to analyze, while background rejection helps identify which signals are plausibly neutrino-related. These are complementary needs: volume alone does not identify an event, and careful analysis cannot recover interactions that never happened in the instrument.
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What can supernova neutrinos tell us?
Neutrinos can escape from a stellar explosion and reach detectors as a short-lived burst, offering information about the event that is difficult to obtain from light alone. Fermilab estimates that about 99 percent of a supernova’s energy is carried away by neutrinos over roughly 10 seconds. For a supernova in our galaxy, the same source estimates that one detector could record 5,000 to 8,000 events. Those figures are estimates from Fermilab’s supernova-neutrino page, not a guaranteed count for every detector or every supernova.
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