Introduction
The unfolding of the physics of neutrinos has been a premier scientific achievement of the 20th century. The hallmark of this decades-long endeavor has been the intertwined contributions of experiment and theory in its advancement. This fascinating history has been the subject of many treatises. Our aim is to give an overview of the aggregate knowledge of neutrino physics today and to mark future pathways for still deeper understanding. In this enterprise we bring together, under one broad umbrella, what has been learned and what is now being pursued about neutrinos in a diversity of subareasâparticle physics, nuclear physics, astrophysics, and cosmology. Neutrinos are of key importance in understanding the nature of our universe and there is a new synergy of these branches of physics in their study. A brief flashback to major milestones along the road of neutrino discovery is an appropriate beginning and the subject of this introduction.
The nuclear model of the atom circa 1930 was atomic electrons bound to a positive nucleus by the electromagnetic force. The nucleus was believed to be composed of both protons and electrons, in numbers such that the atomic number
A and the nuclear charge
Z were accounted for. A challenge to this description was that radioactive nuclei were observed to undergo spontaneous beta-decay
A â
AâČ +
e. By energy and momentum conservation, all the emitted electrons should have the same energy, but a continuous electron energy spectrum was observed. This totally unexpected phenomenon caused both Niels Bohr and Paul Dirac to consider the extreme possibility that energy was not conserved. Another apparent difficulty of the nuclear model was the âfalseâ statistics of the
14N and
19Li nuclei. Because
14N has 7 atomic electrons, its nucleus, supposedly consisting of 14 protons and 7 electrons, should have spin-
, but scattering experiments showed it to have integer spin. Wolfgang Pauli of Eidgenössische Technische Hochschule (ETH), Zurich, saw a way out of this conundrum. He proposed, in a letter to a conference that he was unable to attend, his desperate remedy: nuclei also have very light neutral constituents of spin-
, which he called neutrons [
1]. His neutrons could solve the spin-statistics problem and explain the continuous beta spectrum, since the neutrons would be emitted in conjunction with electrons,
A â
AâČ +
e +
n, so the energy spectrum of the emitted electrons would not be monoenergetic. To be consistent with the observed
electron energy sprectrum, the mass of his neutron had to be less than one percent of the proton mass. Pauli was embarrassed by his rash proposal because he thought that his neutron could never be detected, because of the weakness of its interaction. Pauliâs nuclear model was complex: the nucleus would consist of protons, electrons, and neutrons: e.g., 14 protons, 7 electrons, and 7 neutrons in the
14N nucleus.
In 1932 James Chadwick, then at the Cavendish Laboratory of the University of Cambridge in England, discovered the neutron [2], but it was not the weakly interacting particle emitted in beta decays. Instead, the neutron was a strongly interacting neutral companion of the proton, and the nuclear model simplified to protons and neutrons bound by the strong force: 7 protons and 7 neutrons in the 14N nucleus.
In 1934 Enrico Fermi, then at the University of Rome, reformulated Pauliâs idea that a very light neutral particle was involved in radioactive decays. He renamed it the neutrino (the âlittle neutral oneâ in Italian). In his famous theory of beta decay [
3], Fermi invoked antiparticles (predicted by Dirac in 1931), Pauliâs emitted particle (the antineutrino), and quantum field theory (in which particles can be destroyed or created). In the weak interaction according to Fermi, neutrons decay to protons via a nonrenormalizable four-fermion interaction,
n â
p +
eâ +
e where
e is the electron-antineutrino. The electron and the antineutrino are created as a pair, rather than being emitted from the nucleus. Moreover, the process obtained by crossing initial and final lines in a Feynman diagram have the same strength. Thus, Fermiâs theory predicts the inverse process
e +
p â
e+ +
n, with an interaction of the same strength as that of neutron decay. The reality of the neutrino could thus be tested by observing this inverse reaction with an intense neutrino beta decay source from reactors.
In 1955,
e scattering events were observed by Frederick Reines and Clyde Cowan, Jr., American physicists working at the Los Alamos National Laboratory, via the inverse beta decay process in an experiment at the Savannah River reactor in South Carolina [
4]. The reactor provided an intense antineutrino flux of 5 Ă 10
13/cm
2/s. Scintillators in a tank of water were used to observe the oppositely directed gamma rays from positron annihilations and a time-delayed (by 200
ÎŒs) 2.2 MeV gamma ray from the capture of the neutron on cadmium in the water. The measured inverse beta decay cross section was later found to be consistent with the prediction, indicating that the antineutrinos had been detected.
In 1956, T. D. Lee of Columbia University and C. N. Yang, then of Brookhaven National Laboratory (BNL), interpreted the decays of two species of neutral kaons observed in experiments at BNL as a breakdown of the law of parity (P) conservation (invariance under spatial inversion) [5]. They suggested radioactive beta-decay experiments as a further test. Shortly thereafter, C. S. Wu of Columbia University carried out an experiment on the radioactive beta decays of 60Co that confirmed parity violation [6].
The idea of a maximal parity violating VâA chiral structure of the weak interaction (with vector and axial vector currents of equal strength) originated in 1957â1958 by George Sudarshan and Robert Marshak [7], of Harvard University and the University of Rochester, respectively, and by Richard Feynman and Murray Gell-Mann [8], of Caltech, at a time when some experiments favored a scalar-tensor interaction. According to the V â A theory the neutrino is left-handed and the antineutrino is right-handed. This was confirmed in 1958 by Maurice Goldhaber, Lee Grodzins, and Andrew Sunyar at BNL by studying the circular polarization and resonant scattering of gamma rays following orbital electron capture in a metastable state of 152Eu [9].
A major experimental leap forward occurred in 1962, when a team led by Leon Lederman, Melvin Schwartz, and Jack Steinberger used charged pions produced by the Alternating Gradient Synchrotron at the BNL to establish the existence of the muon-neutrino (ΜΌ) [10]. Charged pions decay dominantly to muons and an associated neutrino. The interactions of these neutrinos in a 10-ton spark chamber were found to produce muons but not electrons.
In 1964, James Cronin and Val Fitch showed that, in the decays of the particles called neutral kaons, not only was the parity symmetry violated, but also the combination CP was violated [11], where C is the charge conjugation symmetry. This CP symmetry breaking is very small but could have created an initial asymmetry between matter and antimatter at the beginning of the universe (at the level of one part in a billion), which after matter-antimatter annihilation leads to the preponderance of matter in the known universe [12]. In the last decade, the BaBar [13] and Belle [14] experiments have shown that CP is violated in the B mesons decays, and much more strongly.
The question of whether neutrinos had mass persisted for decades. A direct probe is the energy spectrum of the electron emitted in beta decay, since a finite neutrino mass would cause a truncation of the spectrum at its endpoint. Experiments on tritium beta decays placed increasingly more restrictive upper bounds and currently restrict the neutrino mass to be less than a few electron-volts [15, 16].
The prescient idea of neutrino oscillations was made by Bruno Pontecorvo in 1957 [
17], who proposed the idea of transitions between neutrinos and antineutrinos as an analogy to the
oscillations observed in the neutral kaon system. This process later became known as oscillat...