Neutrino

Neutrino/Antineutrino
FirstNeutrinoEventAnnotated.jpg
The first use of a hydrogen bubble chamber to detect neutrinos, on 13 November 1970, 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.
CompositionElementary particle
StatisticsFermionic
GenerationFirst, second and third
InteractionsWeak interaction and gravitation
Symbol
ν
e
,
ν
μ
,
ν
τ
,
ν
e
,
ν
μ
,
ν
τ
AntiparticleOpposite chirality from particle
Theorized

  • ν
    e
    , electron neutrino: Wolfgang Pauli (1930)

  • ν
    μ
    , muon neutrino: late 1940s

  • ν
    τ
    , tau neutrino: mid-1970s
Discovered
Types3: electron neutrino, muon neutrino, and tau neutrino
Mass<0.120 eV/c2 (<2.14 × 10−37 kg), 95% confidence level, sum of 3 flavors[1]
Electric chargee
Spin1/2
Weak isospinLH: +1/2, RH: 0
Weak hyperchargeLH: −1, RH: 0
BL−1
X−3

A neutrino (/ or /) (denoted by the Greek letter ν) is a fermion (an elementary particle with 2) that interacts only via the weak subatomic force and gravity.[2][3] The neutrino is so named because it is electrically neutral and because its rest mass is so small (-ino) that it was long thought to be zero. The mass of the neutrino is much smaller than that of the other known elementary particles.[1] The weak force has a very short range, the gravitational interaction is extremely weak, and neutrinos do not participate in the strong interaction. Thus, neutrinos typically pass through normal matter unimpeded and undetected.[2][3]

Weak interactions create neutrinos in one of three leptonic flavors: electron neutrinos (
ν
e
),
muon neutrinos (
ν
μ
), or tau neutrinos (
ν
τ
), in association with the corresponding charged lepton.[4] Although neutrinos were long believed to be massless, it is now known that there are three discrete neutrino masses with different tiny values, but they do not correspond uniquely to the three flavors. A neutrino created with a specific flavor has an associated specific quantum superposition of all three mass states. As a result, neutrinos oscillate between different flavors in flight. For example, an electron neutrino produced in a beta decay reaction may interact in a distant detector as a muon or tau neutrino.[5][6] Although only differences between squares of the three mass values are known as of 2019,[7] cosmological observations imply that the sum of the three masses must be less than one millionth that of the electron.[1][8]

For each neutrino, there also exists a corresponding antiparticle, called an antineutrino, which also has spin of 1/2 and no electric charge. Antineutrinos are distinguished from the neutrinos by having opposite signs of lepton number and right-handed instead of left-handed chirality. To conserve total lepton number (in nuclear beta decay), electron neutrinos only appear together with positrons (anti-electrons) or electron-antineutrinos, whereas electron antineutrinos only appear with electrons or electron neutrinos.[9][10]

Neutrinos are created by various radioactive decays; the following list is not exhaustive, but includes some of those processes:

The majority of neutrinos which are detected about the Earth are from nuclear reactions inside the Sun.

At the surface of our planet, about 65 billion (6.5×1010) solar neutrinos pass, per second per square centimeter; laterally (that is perpendicularly to the direction of the sun).[11][12]

Research is intense in the hunt to elucidate the quintessential nature of neutrinos, with aspirations in order to determine: the three neutrino mass values, the measurement of the degree of CP violation in the leptonic sector (which may lead to leptogenesis); and searches for evidence of physics which might break the Standard Model of particle physics, such as neutrinoless double beta decay, which would be evidence for violation of lepton number conservation. Neutrinos can also be used for tomography of the interior of the earth.[13][14]

History

Pauli's proposal

The neutrino[a] was postulated first by Wolfgang Pauli in 1930 to explain how beta decay could conserve energy, momentum, and angular momentum (spin). In contrast to Niels Bohr, who proposed a statistical version of the conservation laws to explain the observed continuous energy spectra in beta decay, Pauli hypothesized an undetected particle that he called a "neutron", using the same -on ending employed for naming both the proton and the electron. He considered that the new particle was emitted from the nucleus together with the electron or beta particle in the process of beta decay.[15][b]

James Chadwick discovered a much more massive neutral nuclear particle in 1932 and named it a neutron also, leaving two kinds of particles with the same name. Earlier (in 1930) Pauli had used the term "neutron" for both the neutral particle that conserved energy in beta decay, and a presumed neutral particle in the nucleus; initially he did not consider these two neutral particles as distinct from each other.[15] The word "neutrino" entered the scientific vocabulary through Enrico Fermi, who used it during a conference in Paris in July 1932 and at the Solvay Conference in October 1933, where Pauli also employed it. The name (the Italian equivalent of "little neutral one") was jokingly coined by Edoardo Amaldi during a conversation with Fermi at the Institute of Physics of via Panisperna in Rome, in order to distinguish this light neutral particle from Chadwick's heavy neutron.[16]

In Fermi's theory of beta decay, Chadwick's large neutral particle could decay to a proton, electron, and the smaller neutral particle (now called an electron antineutrino):


n0

p+
+
e
+
ν
e

Fermi's paper, written in 1934, unified Pauli's neutrino with Paul Dirac's positron and Werner Heisenberg's neutron–proton model and gave a solid theoretical basis for future experimental work. The journal Nature rejected Fermi's paper, saying that the theory was "too remote from reality". He submitted the paper to an Italian journal, which accepted it, but the general lack of interest in his theory at that early date caused him to switch to experimental physics.[17]:24[18]

By 1934 there was experimental evidence against Bohr's idea that energy conservation is invalid for beta decay: At the Solvay conference of that year, measurements of the energy spectra of beta particles (electrons) were reported, showing that there is a strict limit on the energy of electrons from each type of beta decay. Such a limit is not expected if the conservation of energy is invalid, in which case any amount of energy would be statistically available in at least a few decays. The natural explanation of the beta decay spectrum as first measured in 1934 was that only a limited (and conserved) amount of energy was available, and a new particle was sometimes taking a varying fraction of this limited energy, leaving the rest for the beta particle. Pauli made use of the occasion to publicly emphasize that the still-undetected "neutrino" must be an actual particle.[17]:25

Direct detection

Clyde Cowan conducting the neutrino experiment circa 1956

In 1942, Wang Ganchang first proposed the use of beta capture to experimentally detect neutrinos.[19] In the 20 July 1956 issue of Science, Clyde Cowan, Frederick Reines, F. B. Harrison, H. W. Kruse, and A. D. McGuire published confirmation that they had detected the neutrino,[20][21] a result that was rewarded almost forty years later with the 1995 Nobel Prize.[22]

In this experiment, now known as the Cowan–Reines neutrino experiment, antineutrinos created in a nuclear reactor by beta decay reacted with protons to produce neutrons and positrons:


ν
e
+
p+

n0
+
e+

The positron quickly finds an electron, and they annihilate each other. The two resulting gamma rays (γ) are detectable. The neutron can be detected by its capture on an appropriate nucleus, releasing a gamma ray. The coincidence of both events – positron annihilation and neutron capture – gives a unique signature of an antineutrino interaction.

In February 1965, the first neutrino found in nature was identified in one of South Africa's gold mines by a group which included Friedel Sellschop.[23] The experiment was performed in a specially prepared chamber at a depth of 3 km in the ERPM mine near Boksburg. A plaque in the main building commemorates the discovery. The experiments also implemented a primitive neutrino astronomy and looked at issues of neutrino physics and weak interactions.[24]

Neutrino flavor

The antineutrino discovered by Cowan and Reines is the antiparticle of the electron neutrino.

In 1962, Leon M. Lederman, Melvin Schwartz and Jack Steinberger showed that more than one type of neutrino exists by first detecting interactions of the muon neutrino (already hypothesised with the name neutretto),[25] which earned them the 1988 Nobel Prize in Physics.

When the third type of lepton, the tau, was discovered in 1975 at the Stanford Linear Accelerator Center, it was also expected to have an associated neutrino (the tau neutrino). First evidence for this third neutrino type came from the observation of missing energy and momentum in tau decays analogous to the beta decay leading to the discovery of the electron neutrino. The first detection of tau neutrino interactions was announced in 2000 by the DONUT collaboration at Fermilab; its existence had already been inferred by both theoretical consistency and experimental data from the Large Electron–Positron Collider.[26]

Solar neutrino problem

In the 1960s, the now-famous Homestake experiment made the first measurement of the flux of electron neutrinos arriving from the core of the Sun and found a value that was between one third and one half the number predicted by the Standard Solar Model. This discrepancy, which became known as the solar neutrino problem, remained unresolved for some thirty years, while possible problems with both the experiment and the solar model were investigated, but none could be found. Eventually it was realized that both were actually correct, and that the discrepancy between them was due to neutrinos being more complex than was previously assumed. It was postulated that the three neutrinos had nonzero and slightly different masses, and could therefore oscillate into undetectable flavors on their flight to the Earth. This hypothesis was investigated by a new series of experiments, thereby opening a new major field of research that still continues. Eventual confirmation of the phenomenon of neutrino oscillation led to two Nobel prizes, to Raymond Davis, Jr., who conceived and led the Homestake experiment, and to Art McDonald, who led the SNO experiment, which could detect all of the neutrino flavors and found no deficit.[27]

Oscillation

A practical method for investigating neutrino oscillations was first suggested by Bruno Pontecorvo in 1957 using an analogy with kaon oscillations; over the subsequent 10 years he developed the mathematical formalism and the modern formulation of vacuum oscillations. In 1985 Stanislav Mikheyev and Alexei Smirnov (expanding on 1978 work by Lincoln Wolfenstein) noted that flavor oscillations can be modified when neutrinos propagate through matter. This so-called Mikheyev–Smirnov–Wolfenstein effect (MSW effect) is important to understand because many neutrinos emitted by fusion in the Sun pass through the dense matter in the solar core (where essentially all solar fusion takes place) on their way to detectors on Earth.

Starting in 1998, experiments began to show that solar and atmospheric neutrinos change flavors (see Super-Kamiokande and Sudbury Neutrino Observatory). This resolved the solar neutrino problem: the electron neutrinos produced in the Sun had partly changed into other flavors which the experiments could not detect.

Although individual experiments, such as the set of solar neutrino experiments, are consistent with non-oscillatory mechanisms of neutrino flavor conversion, taken altogether, neutrino experiments imply the existence of neutrino oscillations. Especially relevant in this context are the reactor experiment KamLAND and the accelerator experiments such as MINOS. The KamLAND experiment has indeed identified oscillations as the neutrino flavor conversion mechanism involved in the solar electron neutrinos. Similarly MINOS confirms the oscillation of atmospheric neutrinos and gives a better determination of the mass squared splitting.[28] Takaaki Kajita of Japan, and Arthur B. McDonald of Canada, received the 2015 Nobel Prize for Physics for their landmark finding, theoretical and experimental, that neutrinos can change flavors.

Cosmic neutrinos

Raymond Davis, Jr. and Masatoshi Koshiba were jointly awarded the 2002 Nobel Prize in Physics. Both conducted pioneering work on solar neutrino detection, and Koshiba's work also resulted in the first real-time observation of neutrinos from the SN 1987A supernova in the nearby Large Magellanic Cloud. These efforts marked the beginning of neutrino astronomy.[29]

SN 1987A represents the only verified detection of neutrinos from a supernova. However, many stars have gone supernova in the universe, leaving a theorized diffuse supernova neutrino background.

Other Languages
Afrikaans: Neutrino
العربية: نيوترينو
অসমীয়া: নিউট্ৰিন'
asturianu: Neutrín
azərbaycanca: Neytrino
تۆرکجه: نوترینو
беларуская: Нейтрына
български: Неутрино
bosanski: Neutrino
català: Neutrí
čeština: Neutrino
dansk: Neutrino
Deutsch: Neutrino
eesti: Neutriinod
Ελληνικά: Νετρίνο
español: Neutrino
Esperanto: Neŭtrino
euskara: Neutrino
فارسی: نوترینو
français: Neutrino
Frysk: Neutrino
Gaeilge: Neoidríonó
galego: Neutrino
한국어: 중성미자
հայերեն: Նեյտրինո
हिन्दी: न्यूट्रिनो
hrvatski: Neutrino
Bahasa Indonesia: Neutrino
íslenska: Fiseind
italiano: Neutrino
עברית: נייטרינו
қазақша: Нейтрино
Latina: Neutrinum
latviešu: Neitrīno
Lëtzebuergesch: Neutrino
lietuvių: Neutrinas
Limburgs: Neutrino
lumbaart: Neütrin
magyar: Neutrínó
македонски: Неутрино
മലയാളം: ന്യൂട്രിനോ
Bahasa Melayu: Neutrino
မြန်မာဘာသာ: နျူထရီနို
Nederlands: Neutrino
norsk: Nøytrino
norsk nynorsk: Nøytrino
occitan: Neutrinò
oʻzbekcha/ўзбекча: Neytrino
ਪੰਜਾਬੀ: ਨਿਊਟ੍ਰੀਨੋ
پنجابی: نیوٹرینو
Patois: Nyuuchriino
Plattdüütsch: Neutrino
polski: Neutrino
português: Neutrino
română: Neutrin
русский: Нейтрино
sardu: Neutrino
Scots: Neutrino
Seeltersk: Neutrino
sicilianu: Niutrìnu
Simple English: Neutrino
slovenčina: Neutríno
slovenščina: Nevtrino
српски / srpski: Неутрино
srpskohrvatski / српскохрватски: Neutrino
suomi: Neutriino
svenska: Neutrino
татарча/tatarça: Neytrino
తెలుగు: న్యూట్రినో
Türkçe: Nötrino
українська: Нейтрино
Tiếng Việt: Neutrino
Winaray: Neutrino
吴语: 中微子
粵語: 微中子
中文: 中微子
kriyòl gwiyannen: Nétrino