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Neutrinos come from natural processes such as the Sun, exploding stars, radioactive decay and interactions in Earth’s atmosphere—and from human-made sources such as nuclear reactors and particle accelerators. Because they interact so rarely, detectors do not photograph neutrinos passing by: they record light or other signals from particles created when a neutrino does interact.
Where do neutrinos come from?
Neutrinos are produced in nuclear reactions and particle decays. Their sources include stars, radioactive materials and energetic particle collisions. Fermilab lists Earth, the Sun, stellar explosions, the early universe, atmospheric interactions and radioactive processes among natural sources. Reactors and accelerator beams provide controlled human-made sources. Fermilab’s overview of neutrino sources describes these origins.
The Sun
Fusion in the Sun produces solar neutrinos. Because they escape the Sun and travel to Earth, measuring them gives scientists a way to study solar reactions. Historical solar-neutrino measurements also helped bring neutrino oscillations—the transformation of one neutrino type into another—into focus. Fermilab’s solar-neutrino explanation covers their connection to fusion and oscillations.
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Cosmic rays striking Earth’s atmosphere create particle cascades that produce atmospheric neutrinos. Radioactive processes also produce neutrinos. These sources are useful to experiments because they provide neutrinos without a nearby reactor or accelerator beam.
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Reactors and accelerator beams
Nuclear reactors produce neutrinos as a by-product of nuclear reactions. Particle accelerators can generate beams from particle decays, giving researchers a more controlled source whose direction and production can be studied. This makes it possible to investigate neutrino behavior over a known path and compare results with other sources.
Exploding stars and other astrophysical sources
Supernovae release a large share of their energy as neutrinos. Unlike the steady flow from the Sun, a nearby supernova would produce a brief burst that detectors could observe. Neutrinos also originate in the early universe and other energetic astrophysical environments.
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How do scientists detect neutrinos?
Neutrinos have no electric charge and interact very rarely with matter. Most pass through a detector without leaving a record. On the uncommon occasion that one interacts, it can produce a charged particle. That secondary particle may create light, a track, bubbles or another measurable signal in the detector material. Scientists infer the neutrino’s presence and properties from those effects rather than capturing an image of the neutrino itself. Fermilab’s detection FAQ explains this indirect method.
Because interactions are rare, experiments need substantial amounts of target material and long observation periods to collect useful numbers of events. They also have to distinguish neutrino signals from other particles and sources of background. Detector size, sensor design, location and analysis methods all help with that task.
Why are neutrino detectors so big?
A larger detector contains more material in which a neutrino might interact, increasing the chance of recording an event. Long-running experiments gather more opportunities as well. But size alone is not enough: researchers must identify which recorded signals are consistent with neutrino interactions and reject backgrounds. The best detector design depends on the source and energy range being studied.
How do IceCube and Super-Kamiokande detect neutrinos?
Both experiments detect signals made by secondary particles, but they use different materials and sensor arrangements. Those choices suit different observation goals; the facilities are not interchangeable versions of the same instrument.
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| Experiment | Detection material and sensors | Sources or energy information in the cited descriptions | Recorded signal |
|---|---|---|---|
| IceCube | Optical sensors embedded in Antarctic ice | Its main array is described as most sensitive above the teraelectronvolt scale. DeepCore extends sensitivity to lower energies; the IceCube Masterclass page states a lower reach of 50 GeV. | Light from charged secondary particles created in neutrino interactions |
| Super-Kamiokande | Water viewed by photomultiplier tubes | Studies solar, atmospheric and accelerator-produced neutrinos | Light and its timing, used to analyze particle events |
The IceCube energy descriptions are specific to the detector overview and DeepCore, not universal thresholds for neutrino detection. See the IceCube Masterclass explanation and NASA’s IceCube observatory page. For Super-Kamiokande, see its official detector description and experiment overview.
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IceCube uses the Antarctic ice sheet as its detection medium. Optical modules buried in the ice record light produced by charged particles after neutrino interactions. Its DeepCore subdetector improves sensitivity at lower energies than the main array. The cited Masterclass description gives DeepCore’s lower reach as 50 GeV and characterizes the main array’s major sensitivity as above the TeV scale.
Super-Kamiokande: light in water
Super-Kamiokande is a water Cherenkov detector. Photomultiplier tubes record light and timing information from particle events in the water. The experiment studies neutrinos from the Sun, atmosphere and accelerator beams. Its official overview associates atmospheric-neutrino observations in 1998 with the discovery of neutrino oscillation.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.What can a supernova neutrino signal tell us?
Neutrinos can escape from a supernova while the star’s explosion is unfolding, making them a valuable signal of the event’s interior processes. Fermilab’s supernova-neutrino page estimates that roughly 99 percent of a supernova’s energy is carried away by neutrinos over about 10 seconds. It also estimates 5,000 to 8,000 events in one detector for a supernova in our galaxy. These are the page’s estimates, not a guaranteed count for every detector or every supernova. Fermilab’s supernova-neutrino page provides the figures.
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