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As of , no evidence has been found for any other difference. So far, despite extensive and continuing searches for exceptions, in all observed leptonic processes there has never been any change in total lepton number; for example, if the total lepton number is zero in the initial state, then the final state has only matched lepton and anti-lepton pairs: electron neutrinos appear in the final state together with only positrons anti-electrons or electron antineutrinos, and electron antineutrinos with electrons or electron neutrinos.
Antineutrinos are produced in nuclear beta decay together with a beta particle in beta decay a neutron decays into a proton, electron, and antineutrino. All antineutrinos observed thus far had right-handed helicity i. Antineutrinos were first detected as a result of their interaction with protons in a large tank of water.
This was installed next to a nuclear reactor as a controllable source of the antineutrinos see Cowan—Reines neutrino experiment. Researchers around the world have begun to investigate the possibility of using antineutrinos for reactor monitoring in the context of preventing the proliferation of nuclear weapons.
Because antineutrinos and neutrinos are neutral particles, it is possible that they are the same particle. Particles that have this property are known as Majorana particles , named after the Italian physicist Ettore Majorana who first proposed the concept.
For the case of neutrinos this theory has gained popularity as it can be used, in combination with the seesaw mechanism , to explain why neutrino masses are so small compared to those of the other elementary particles, such as electrons or quarks. Majorana neutrinos would have the property that the neutrino and antineutrino could be distinguished only by chirality ; what experiments observe as a difference between the neutrino and antineutrino could simply be due to one particle with two possible chiralities.
As of [update] , it is not known whether neutrinos are Majorana or Dirac particles. It is possible to test this property experimentally. For example, if neutrinos are indeed Majorana particles, then lepton-number violating processes such as neutrinoless double beta decay would be allowed, while they would not if neutrinos are Dirac particles. Several experiments have been and are being conducted to search for this process, e. Neutrinos can interact with a nucleus, changing it to another nucleus.
This process is used in radiochemical neutrino detectors. In this case, the energy levels and spin states within the target nucleus have to be taken into account to estimate the probability for an interaction. In general the interaction probability increases with the number of neutrons and protons within a nucleus. It is very hard to uniquely identify neutrino interactions among the natural background of radioactivity.
For this reason, in early experiments a special reaction channel was chosen to facilitate the identification: the interaction of an antineutrino with one of the hydrogen nuclei in the water molecules. A hydrogen nucleus is a single proton, so simultaneous nuclear interactions, which would occur within a heavier nucleus, don't need to be considered for the detection experiment.
Within a cubic metre of water placed right outside a nuclear reactor, only relatively few such interactions can be recorded, but the setup is now used for measuring the reactor's plutonium production rate. Very much like neutrons do in nuclear reactors , neutrinos can induce fission reactions within heavy nuclei. The process affects the abundance of isotopes seen in the universe. The current best measurement of the number of neutrino types comes from observing the decay of the Z boson.
This particle can decay into any light neutrino and its antineutrino, and the more available types of light neutrinos, [d] the shorter the lifetime of the Z boson. Measurements of the Z lifetime have shown that three light neutrino flavors couple to the Z. There are several active research areas involving the neutrino. Some are concerned with testing predictions of neutrino behavior. Other research is focused on measurement of unknown properties of neutrinos; there is special interest in experiments that determine their masses and rates of CP violation , which cannot be predicted from current theory.
International scientific collaborations install large neutrino detectors near nuclear reactors or in neutrino beams from particle accelerators to better constrain the neutrino masses and the values for the magnitude and rates of oscillations between neutrino flavors.
These experiments are thereby searching for the existence of CP violation in the neutrino sector; that is, whether or not the laws of physics treat neutrinos and antineutrinos differently. The KATRIN experiment in Germany began to acquire data in June  to determine the value of the mass of the electron neutrino, with other approaches to this problem in the planning stages.
Despite their tiny masses, neutrinos are so numerous that their gravitational force can influence other matter in the universe. The three known neutrino flavors are the only established elementary particle candidates for dark matter , specifically hot dark matter , although the conventional neutrinos seem to be essentially ruled out as substantial proportion of dark matter based on observations of the cosmic microwave background. It still seems plausible that heavier, sterile neutrinos might compose warm dark matter , if they exist.
Other efforts search for evidence of a sterile neutrino — a fourth neutrino flavor that does not interact with matter like the three known neutrino flavors. Therefore, heavy sterile neutrinos would have a mass of at least The existence of such particles is in fact hinted by experimental data from the LSND experiment.
On the other hand, the currently running MiniBooNE experiment suggested that sterile neutrinos are not required to explain the experimental data,  although the latest research into this area is on-going and anomalies in the MiniBooNE data may allow for exotic neutrino types, including sterile neutrinos. According to an analysis published in , data from the Wilkinson Microwave Anisotropy Probe of the cosmic background radiation is compatible with either three or four types of neutrinos.
Another hypothesis concerns "neutrinoless double-beta decay", which, if it exists, would violate lepton number conservation. Searches for this mechanism are underway but have not yet found evidence for it. If they were to, then what are now called antineutrinos could not be true antiparticles. Cosmic ray neutrino experiments detect neutrinos from space to study both the nature of neutrinos and the cosmic sources producing them.
Before neutrinos were found to oscillate, they were generally assumed to be massless, propagating at the speed of light c. According to the theory of special relativity , the question of neutrino velocity is closely related to their mass : If neutrinos are massless, they must travel at the speed of light, and if they have mass they cannot reach the speed of light.
Due to their tiny mass, the predicted speed is extremely close to the speed of light in all experiments, and current detectors are not sensitive to the expected difference. Also, there are some Lorentz-violating variants of quantum gravity which might allow faster-than-light neutrinos. The first measurements of neutrino speed were made in the early s using pulsed pion beams produced by pulsed proton beams hitting a target.
The pions decayed producing neutrinos, and the neutrino interactions observed within a time window in a detector at a distance were consistent with the speed of light. The central value of 1. A similar observation was made, on a much larger scale, with supernova A SN A. Antineutrinos with an energy of 10 MeV from the supernova were detected within a time window that was consistent with the speed of light for the neutrinos.
So far, all measurements of neutrino speed have been consistent with the speed of light. In November , OPERA repeated its experiment with changes so that the speed could be determined individually for each detected neutrino. The results showed the same faster-than-light speed.
In February , reports came out that the results may have been caused by a loose fiber optic cable attached to one of the atomic clocks which measured the departure and arrival times of the neutrinos. An independent recreation of the experiment in the same laboratory by ICARUS found no discernible difference between the speed of a neutrino and the speed of light. Can we measure the neutrino masses? Do neutrinos follow Dirac or Majorana statistics? The Standard Model of particle physics assumed that neutrinos are massless.
Enhancing the basic framework to accommodate their mass is straightforward by adding a right-handed Lagrangian. The strongest upper limit on the masses of neutrinos comes from cosmology : the Big Bang model predicts that there is a fixed ratio between the number of neutrinos and the number of photons in the cosmic microwave background.
If the total energy of all three types of neutrinos exceeded an average of 50 eV per neutrino, there would be so much mass in the universe that it would collapse. A much more stringent constraint comes from a careful analysis of cosmological data, such as the cosmic microwave background radiation, galaxy surveys , and the Lyman-alpha forest.
Analysis of data from the WMAP microwave space telescope found that the sum of the masses of the three neutrino species must be less than 0. McDonald for their experimental discovery of neutrino oscillations, which demonstrates that neutrinos have mass. In , research results at the Super-Kamiokande neutrino detector determined that neutrinos can oscillate from one flavor to another, which requires that they must have a nonzero mass.
This is because neutrino oscillations are sensitive only to the difference in the squares of the masses. Thus, there exists at least one neutrino mass eigenstate with a mass of at least 0. A number of efforts are under way to directly determine the absolute neutrino mass scale in laboratory experiments, especially using nuclear beta decay.
Upper limits on the effective electron neutrino masses come from beta decays of tritium. On 31 May , OPERA researchers observed the first tau neutrino candidate event in a muon neutrino beam, the first time this transformation in neutrinos had been observed, providing further evidence that they have mass.
If the neutrino is a Majorana particle , the mass may be calculated by finding the half-life of neutrinoless double-beta decay of certain nuclei. Since the neutrino is an elementary particle it does not have a size in the same sense as everyday objects: Like all other Standard Model fundamental particles, neutrinos are point-like, with neither width nor volume. In one sense, particles with mass have a wavelength the Compton wavelength which is useful for estimating their cross-sections for collisions.
The smaller a particle's mass, the larger its Compton wavelength. Based on the upper limit of 0. This extremely long wavelength for a particle with mass leads physicists to suspect that even though neutrinos follow Fermi statistics , that their behavior may be much like a wave, making them seem Bosonic , and thus placing them near the border between particles fermions and waves bosons.
Experimental results show that within the margin of error, all produced and observed neutrinos have left-handed helicities spins antiparallel to momenta , and all antineutrinos have right-handed helicities. These are the only chiralities included in the Standard Model of particle interactions.
It is possible that their counterparts right-handed neutrinos and left-handed antineutrinos simply do not exist. If they do exist, their properties are substantially different from observable neutrinos and antineutrinos. It is theorized that they are either very heavy on the order of GUT scale —see Seesaw mechanism , do not participate in weak interaction so-called sterile neutrinos , or both. The existence of nonzero neutrino masses somewhat complicates the situation.
Neutrinos are produced in weak interactions as chirality eigenstates. Chirality of a massive particle is not a constant of motion; helicity is, but the chirality operator does not share eigenstates with the helicity operator. This does not significantly affect the experiments, because neutrinos involved are nearly always ultrarelativistic, and thus mixing amplitudes are vanishingly small. Effectively, they travel so quickly and time passes so slowly in their rest-frames that they do not have enough time to change over any observable path.
For example, most solar neutrinos have energies on the order of 0. An unexpected series of experimental results for the rate of decay of heavy highly charged radioactive ions circulating in a storage ring has provoked theoretical activity in an effort to find a convincing explanation.
The rates of weak decay of two radioactive species with half lives of about 40 seconds and seconds were found to have a significant oscillatory modulation , with a period of about 7 seconds. Ideas related to flavour oscillation met with skepticism. Nuclear reactors are the major source of human-generated neutrinos.
Including these subsequent decays, the average nuclear fission releases about MeV of energy, of which roughly For a typical nuclear reactor with a thermal power of MW , [e] the total power production from fissioning atoms is actually MW , of which MW is radiated away as antineutrino radiation and never appears in the engineering. This is to say, MW of fission energy is lost from this reactor and does not appear as heat available to run turbines, since antineutrinos penetrate all building materials practically without interaction.
The antineutrino energy spectrum depends on the degree to which the fuel is burned plutonium fission antineutrinos on average have slightly more energy than those from uranium fission , but in general, the detectable antineutrinos from fission have a peak energy between about 3. Only antineutrinos with an energy above threshold of 1. Some particle accelerators have been used to make neutrino beams.
The technique is to collide protons with a fixed target, producing charged pions or kaons. These unstable particles are then magnetically focused into a long tunnel where they decay while in flight. Because of the relativistic boost of the decaying particle, the neutrinos are produced as a beam rather than isotropically. Efforts to design an accelerator facility where neutrinos are produced through muon decays are ongoing.
Nuclear weapons also produce very large quantities of neutrinos. Fred Reines and Clyde Cowan considered the detection of neutrinos from a bomb prior to their search for reactor neutrinos; a fission reactor was recommended as a better alternative by Los Alamos physics division leader J. Neutrinos are produced together with the natural background radiation. In particular, the decay chains of U and Th isotopes, as well as 40 K , include beta decays which emit antineutrinos. These so-called geoneutrinos can provide valuable information on the Earth's interior.
Atmospheric neutrinos result from the interaction of cosmic rays with atomic nuclei in the Earth's atmosphere , creating showers of particles, many of which are unstable and produce neutrinos when they decay. Solar neutrinos originate from the nuclear fusion powering the Sun and other stars.
The details of the operation of the Sun are explained by the Standard Solar Model. In short: when four protons fuse to become one helium nucleus, two of them have to convert into neutrons, and each such conversion releases one electron neutrino. The Sun sends enormous numbers of neutrinos in all directions. Each second, about 65 billion 6.
Mann  found a second and more profuse neutrino source is the thermal energy billion kelvins of the newly formed neutron core, which is dissipated via the formation of neutrino—antineutrino pairs of all flavors. Colgate and White's theory of supernova neutrino production was confirmed in , when neutrinos from Supernova A were detected.
The neutrino signal from the supernova arrived at Earth several hours before the arrival of the first electromagnetic radiation, as expected from the evident fact that the latter emerges along with the shock wave. The exceptionally feeble interaction with normal matter allowed the neutrinos to pass through the churning mass of the exploding star, while the electromagnetic photons were slowed.
Because neutrinos interact so little with matter, it is thought that a supernova's neutrino emissions carry information about the innermost regions of the explosion. Much of the visible light comes from the decay of radioactive elements produced by the supernova shock wave, and even light from the explosion itself is scattered by dense and turbulent gases, and thus delayed.
The neutrino burst is expected to reach Earth before any electromagnetic waves, including visible light, gamma rays, or radio waves. The exact time delay of the electromagnetic waves' arrivals depends on the velocity of the shock wave and on the thickness of the outer layer of the star. For a Type II supernova, astronomers expect the neutrino flood to be released seconds after the stellar core collapse, while the first electromagnetic signal may emerge hours later, after the explosion shock wave has had time to reach the surface of the star.
The Supernova Early Warning System project uses a network of neutrino detectors to monitor the sky for candidate supernova events; the neutrino signal will provide a useful advance warning of a star exploding in the Milky Way. Although neutrinos pass through the outer gases of a supernova without scattering, they provide information about the deeper supernova core with evidence that here, even neutrinos scatter to a significant extent.
In a supernova core the densities are those of a neutron star which is expected to be formed in this type of supernova ,  becoming large enough to influence the duration of the neutrino signal by delaying some neutrinos. The 13 second-long neutrino signal from SN A lasted far longer than it would take for unimpeded neutrinos to cross through the neutrino-generating core of a supernova, expected to be only kilometers in diameter for SN A.
The number of neutrinos counted was also consistent with a total neutrino energy of 2. In addition to the detection of neutrinos from individual supernovae, it should also be possible to detect the diffuse supernova neutrino background , which originates from all supernovae in the Universe. The energy of supernova neutrinos ranges from a few to several tens of MeV. The sites where cosmic rays are accelerated are expected to produce neutrinos that are at least one million times more energetic, produced from turbulent gaseous environments left over by supernova explosions: Supernova remnants.
The origin of the cosmic rays was attributed to supernovas by Baade and Zwicky ; this hypothesis was refined by Ginzburg and Syrovatsky who attributed the origin to supernova remnants, and supported their claim by the crucial remark, that the cosmic ray losses of the Milky Way is compensated, if the efficiency of acceleration in supernova remnants is about 10 percent. Ginzburg and Syrovatskii's hypothesis is supported by the specific mechanism of "shock wave acceleration" happening in supernova remnants, which is consistent with the original theoretical picture drawn by Enrico Fermi , and is receiving support from observational data.
The very high-energy neutrinos are still to be seen, but this branch of neutrino astronomy is just in its infancy. Indeed, the collisions of cosmic rays are supposed to produce charged pions, whose decay give the neutrinos, neutral pions, and gamma rays the environment of a supernova remnant, which is transparent to both types of radiation. Still-higher-energy neutrinos, resulting from the interactions of extragalactic cosmic rays, could be observed with the Pierre Auger Observatory or with the dedicated experiment named ANITA.
It is thought that, just like the cosmic microwave background radiation leftover from the Big Bang , there is a background of low-energy neutrinos in our Universe. In the s it was proposed that these may be the explanation for the dark matter thought to exist in the universe. Neutrinos have one important advantage over most other dark matter candidates: They are known to exist.
This idea also has serious problems. From particle experiments, it is known that neutrinos are very light. This means that they easily move at speeds close to the speed of light. For this reason, dark matter made from neutrinos is termed " hot dark matter ". The problem is that being fast moving, the neutrinos would tend to have spread out evenly in the universe before cosmological expansion made them cold enough to congregate in clumps.
This would cause the part of dark matter made of neutrinos to be smeared out and unable to cause the large galactic structures that we see. These same galaxies and groups of galaxies appear to be surrounded by dark matter that is not fast enough to escape from those galaxies.
Presumably this matter provided the gravitational nucleus for formation. This implies that neutrinos cannot make up a significant part of the total amount of dark matter. From cosmological arguments, relic background neutrinos are estimated to have density of 56 of each type per cubic centimeter and temperature 1. Although their density is quite high, they have not yet been observed in the laboratory, as their energy is below thresholds of most detection methods, and due to extremely low neutrino interaction cross-sections at sub-eV energies.
In contrast, boron-8 solar neutrinos — which are emitted with a higher energy — have been detected definitively despite having a space density that is lower than that of relic neutrinos by some 6 orders of magnitude. Neutrinos cannot be detected directly because they do not carry electric charge, which means they do not ionize the materials they pass through.
Other ways neutrinos might affect their environment, such as the MSW effect , do not produce traceable radiation. A unique reaction to identify antineutrinos, sometimes referred to as inverse beta decay , as applied by Reines and Cowan see below , requires a very large detector to detect a significant number of neutrinos. All detection methods require the neutrinos to carry a minimum threshold energy. So far, there is no detection method for low-energy neutrinos, in the sense that potential neutrino interactions for example by the MSW effect cannot be uniquely distinguished from other causes.
Neutrino detectors are often built underground to isolate the detector from cosmic rays and other background radiation. Antineutrinos were first detected in the s near a nuclear reactor. Reines and Cowan used two targets containing a solution of cadmium chloride in water. Two scintillation detectors were placed next to the cadmium targets. Antineutrinos with an energy above the threshold of 1. The resulting positron annihilation with electrons in the detector material created photons with an energy of about 0.
Pairs of photons in coincidence could be detected by the two scintillation detectors above and below the target. The neutrons were captured by cadmium nuclei resulting in gamma rays of about 8 MeV that were detected a few microseconds after the photons from a positron annihilation event. Since then, various detection methods have been used. Super Kamiokande is a large volume of water surrounded by photomultiplier tubes that watch for the Cherenkov radiation emitted when an incoming neutrino creates an electron or muon in the water.
The Sudbury Neutrino Observatory is similar, but used heavy water as the detecting medium, which uses the same effects, but also allows the additional reaction any-flavor neutrino photo-dissociation of deuterium, resulting in a free neutron which is then detected from gamma radiation after chlorine-capture.
Other detectors have consisted of large volumes of chlorine or gallium which are periodically checked for excesses of argon or germanium , respectively, which are created by electron-neutrinos interacting with the original substance. The IceCube Neutrino Observatory uses 1 km 3 of the Antarctic ice sheet near the south pole with photomultiplier tubes distributed throughout the volume.
Neutrinos' low mass and neutral charge mean they interact exceedingly weakly with other particles and fields. This feature of weak interaction interests scientists because it means neutrinos can be used to probe environments that other radiation such as light or radio waves cannot penetrate. Using neutrinos as a probe was first proposed in the midth century as a way to detect conditions at the core of the Sun. The solar core cannot be imaged directly because electromagnetic radiation such as light is diffused by the great amount and density of matter surrounding the core.
On the other hand, neutrinos pass through the Sun with few interactions. Whereas photons emitted from the solar core may require 40, years to diffuse to the outer layers of the Sun, neutrinos generated in stellar fusion reactions at the core cross this distance practically unimpeded at nearly the speed of light.
Neutrinos are also useful for probing astrophysical sources beyond the Solar System because they are the only known particles that are not significantly attenuated by their travel through the interstellar medium.
Optical photons can be obscured or diffused by dust, gas, and background radiation. High-energy cosmic rays , in the form of swift protons and atomic nuclei, are unable to travel more than about megaparsecs due to the Greisen—Zatsepin—Kuzmin limit GZK cutoff.
Neutrinos, in contrast, can travel even greater distances barely attenuated. The galactic core of the Milky Way is fully obscured by dense gas and numerous bright objects. Neutrinos produced in the galactic core might be measurable by Earth-based neutrino telescopes.
Another important use of the neutrino is in the observation of supernovae , the explosions that end the lives of highly massive stars. The core collapse phase of a supernova is an extremely dense and energetic event.
It is so dense that no known particles are able to escape the advancing core front except for neutrinos. The rest mass of the neutrino is an important test of cosmological and astrophysical theories see Dark matter. The neutrino's significance in probing cosmological phenomena is as great as any other method, and is thus a major focus of study in astrophysical communities.
The study of neutrinos is important in particle physics because neutrinos typically have the lowest mass, and hence are examples of the lowest-energy particles theorized in extensions of the Standard Model of particle physics. In November , American scientists used a particle accelerator to send a coherent neutrino message through feet of rock. This marks the first use of neutrinos for communication, and future research may permit binary neutrino messages to be sent immense distances through even the densest materials, such as the Earth's core.
This is the first time that a neutrino detector has been used to locate an object in space and that a source of cosmic rays has been identified. From Wikipedia, the free encyclopedia. Not to be confused with neutron or neutralino. For other uses, see Neutrino disambiguation. Elementary particle with extremely low mass that interacts only via the weak force and gravity. The first use of a hydrogen bubble chamber to detect neutrinos, on 13 November , at Argonne National Laboratory. Here a neutrino hits a proton in a hydrogen atom; the collision occurs at the point where three tracks emanate on the right of the photograph.
Main article: Solar neutrino problem. Main article: Neutrino oscillation. Main articles: cosmic neutrino background and diffuse supernova neutrino background. Main article: Mikheyev—Smirnov—Wolfenstein effect. Concepts and phenomena. Positron emission tomography Fuel Weapon. People and bodies. See also: Seesaw mechanism. Main article: Measurements of neutrino speed. Main article: Faster-than-light neutrino anomaly. Unsolved problem in physics :. Main article: Sterile neutrino.
Main article: GSI anomaly. Main article: Accelerator neutrinos. Main article: Geoneutrino. Main article: Solar neutrino. Main article: Cosmic neutrino background. Main article: Neutrino detector. Two other types were discovered later: see Neutrino flavor below. Journal of Physics: Conference Series. Bibcode : JPhCS. S2CID Neutrinos softcover ed. Oxford University Press. ISBN The Neutrino Hunters: The chase for the ghost particle and the secrets of the universe softcover ed.
Oneworld Publications. Maybe, just maybe, neutrinos". The New York Times. Retrieved 16 April Chinese Physics C. Physical Review D. Bibcode : PhRvD.. Nuclear Physics B. Bibcode : NuPhB. Particle Data Group Bibcode : ChPhC.. Retrieved 24 April Georgia State University. Boulder, CO: University of Colorado. The Astrophysical Journal.
Bibcode : ApJ American Journal of Physics. Bibcode : AmJPh.. Aartsen; et al. Letter of Intent. Bibcode : arXiv Physics Today. Bibcode : PhT Physics Reports. Bibcode : PhR Bibcode : ZPhy Translated by Wilson, Fred L. Physical Review. Bibcode : PhRv Bibcode : Sci PMID Dj Nejtrino "China Gold". Radio Record Booking:. He won the first place among House Music DJs in Best DJ in according to the London Club.
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