How studying neutrinos can help us to better understand the Universe

Professors Luis A Anchordoqui from City University of New York and Vanderbilt University’s Thomas J Weiler explain how neutrinos can help us to understand the Universe.

The Standard Model (SM) of particle physics is a cornerstone of 20th century physics. It encompasses the first unification of forces in 90 years, since Maxwell unified electricity and magnetism in the early 1880s by noting that the displacement current unified his equation and made magnetism nothing but moving electricity.

The group theory of SM unification can be written as SU(3) × SU(2)L × U(1), with ‘S’ indicating that there are N2 − 1 force particles, one removed from the special (Det = +1) unitary group U(N), while the matter particles of fermions (half-integral quantum mechanical spin) sit in irreducible representations of these three groups. Not included is gravity, which cannot be a gauge theory as it is not renormalisable. Gravity/general relativity is a geometric theory. Thus, we have eight gluons, three W bosons, and a singlet ‘photon’. Adding a complex doublet of Higgs particles to break the SU(2)L × U(1) symmetry completes the SM. The SU(3) is called QCD, short for ‘quantum chromodynamics’, and the SU(2)L × U(1) when suitably broken will contain quantum electrodynamics (or QED) and weak force.

The SM is a renormalisable field theory, which means that the ultraviolet divergences that appear in loop corrections from perturbation theory can be eliminated by a suitable redefinition of the parameters already appearing in the bare Lagrangian: masses, couplings, and field normalisations. The beta function encodes the dependence of a coupling parameter on the energy scale and so the sign of the beta function determines whether an interaction is asymptotically free or enslaved. The beta function depends on the number of vector force particles and the number of matter particles. It turns out that only the SU(3) has a Fermi particle count to yield a positive beta function, indicating that SU(3) = QCD is confining, while unbroken QED and the weak interaction are not.

The strength of the weak interaction rates is given by the ratio (mN/MW)2 ∼ 10−4, where mN is the mass of the nucleon (proton or neutron). In amplitude, the weak interaction extends to ∼ 1/MW, justifying the name ‘weak interaction’. Unification is complete, with the photon arising as the symmetric singlet in the SU(2)L×U(1) interaction. Three Higgses appear as the massive modes of the three massive longitudinal W bosons. There is one Higgs left over. Weak theory and the U(1) have unified as electroweak theory.

Where are the neutrinos?

The neutrinos are in the matter fermions of the SU(2)L chiral symmetry. The symmetry is termed ‘chiral’ because the force field, here massless W bosons, couples to left-handed L fermions but not to right-handed R fermions. L and R are coupled by the mass term. So, for example, we have the electron with its four states to accommodate two spin states and two additional antifermions, but the neutrino, being chargeless, could be its own antiparticle with just two states to accommodate handedness. Does the neutrino consist of two states or four states? I.e., is the neutrino like the electron? Or is it a Majorana fermion, eponymously named after the 1920s physicist who first proposed the self-annihilation of the neutrino? This is an active area of present investigation. One ramification, if the neutrino is Majorana, is neutrinoless double beta decay of two nucleons. A Feynman diagram of this process is shown in Fig. 1.

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Fig 1. The most practical way to uncover the Majorana nature of neutrinos is through the double beta radioactive decay, in which two neutrons simultaneously decay into two protons, releasing two electrons and two electron antineutrinos (left panel). This process has been observed in several different elemental isotopes. However, if neutrinos are Majorana particles, the two released antineutrinos can annihilate each other virtually, yielding ‘neutrinoless double beta decay’ (right panel). Since there are no antineutrinos to carry away any energy, the summed energies of the two electrons should equal the well-known total energy released in the decay. Experiments attempt to observe the antinuetrino annihilation by detecting and summing up the energies of the two released electrons. The summed energy of the two electrons normally has a continuous energy spectrum, because some energy is carried away by the antineutrinos. However, if neutrinos are indeed Majorana, there is also a rare chance for the summed energy of the electrons to equal the total energy loss in the decay. It is this small monoenergtic peak that could become the smoking gun for Majorana particles. The rate is proportional to ∑j mejUej and so only expected to be measurable if j = 3 contains a significant amount of electron neutrino, as in the inverted hierarchy. See main text for details

The symmetry of the vacuum

Sidney Coleman has said that the symmetry of vacuum is the symmetry of the world. In Quantum Field Theory, one may have a vacuum devoid of particles but still containing meaning. So we need to investigate the symmetry of the vacuum. The vacuum has meaning because of Hawking radiation, which in turn is based upon the Heisenberg uncertainty principle. It turns out that energy need not be conserved in physics for tiny times, ∆E ≤ ħ/∆t, where ħ is a fundamental constant of nature (over a 2π) named after Planck.

The physical picture is this: for small times, a fermion pair, such as an electron and positron, may pop out of the vacuum and maintain vacuum quantum numbers as long as it subsequently pops back into the vacuum. The particles are said to be virtual in that they are not observed. In fact, neutrinos are never observed, and therefore always virtual.

The Nobel Prize was awarded a few years back to Takaaki Kajita, director of the SuperK experiment which which initiated measurement of solar neutrinos based on direction of incidence, and succeeded Kamiokande which discovered oscillations in the late 1980s and indicated that neutrinos have a tiny mass; and Arthur McDonald, director of SNOLAB, for the measurement of the electron neutrinos in the Sun which solved the solar issue. Both experiments revealed the unusual behaviour of these misfit particles.

Fig. 2 shows a Cutcosky diagram for neutrino oscillation. The dashed line indicates the cut to of a real axis (on-shell initial and final states). A neutrino of type νµ is produced at the W charged current vertex in association a muon µ. The νµ is virtual. All particles propagate forward in time in mass eigenstates, as shown here for the virtual neutrino. At the lower missing vertex, the neutrino is detected by a second charged current event producing an electron and missing energy. Flavour oscillation has occurred, from an initial νµ to a final state νe. Left of the cut is the quantum amplitude A; right of the cut is A∗. Probability of occurrence is given by AA∗ = |A|2. Note that quantum mechanics is a theory of amplitudes, not of rates.

Mixing and oscillations

In the words of a colleague, the neutrino is as close to nothing as something can be. It is chargeless. Among known interactions, it has only a weak interaction. Formerly believed to be massless, its mass is truly tiny. Quantum mechanics allows one to pick the basis (with some being more useful than others) to describe the survival probability for flavour transitions. We have νj = ∑α Ujανα, where j labels the mass states, α = e,µ,τ are the three neutrino flavours, and U is a large matrix (with elements Ujα) as demonstrated by experiments. ‘Large’ here means the off-diagonal elements are large in appropriate units. No one knows why elements are large, but we got lucky. The neutrino quantum has provided many surprises! Mixing, as with Cabbibo mixing of down and strange quarks, occurs in the Lagrangian. Large mixing in the neutrino sector is a topic under investigation.

Oscillations in space, energy, and time are different from mixing. They are unique to neutrinos and evolve only when masses are degenerate enough to fit inside a single quantum mechanical wave function. They express an interference among mass states which evolves dynamically, meaning in time/energy/position. Oscillation occurs because the three mass state components of the produced flavour travel at slightly different speeds, so that their quantum mechanical wave packets develop relative phase shifts that change how they combine to produce a varying superposition of three flavours. Each flavour component thereby oscillates as the neutrino travels, with the flavours varying in relative strengths. The relative flavour proportions when the neutrino interacts represent the relative probabilities for that flavour of interaction to produce the corresponding flavour of charged lepton. Maki, Nakagawa, and Sakata have chosen the three parameters as angles plus one purely imaginary (the so-called ‘CP phase’) reflecting the fact that U = U† is unitary in quantum mechanics rather than purely real as it is with Euler angles. Remember, it is the complex amplitude that is calculated in quantum mechanics, with the real probability then constructed as P = AA∗ = |A|2. Experiment has shown that three neutrinos are needed for complexity to appear in neutrino physics. And yet we know that oscillations divide into a basis of two 2 x 2 sums, with a ratio of about 30. This is one reason why the complex CP phase is so hard to deduce. From solar neutrino data we furthermore know that ν2 couples with the lighter sum. The question arises: is ν3 heavier than ν2 or lighter? This question is also under investigation. Also under investigation are the mixing angles, e.g. is the largest mixing angle larger or smaller than maximal mixing at 45◦?

Another gift is offered to us by the small neutrino masses, namely the generation of ν masses. Fine tuning of the neutrino’s Yukawa couplings, as is done with all other particles, is a possibility. But the neutrino is known to be five or more orders of magnitude lighter than the next lightest particle, the electron, so an independent mechanism has been invented, the ‘see-saw mechanism’. The see-saw uses properties of a simple 2 x 2 matrix. The matrix lives in neutrino space, with a zero naturally place in the ν-ν 2 × 2 = 3 + 1 (group theory numbers) space, a weak coupling between ν and N (2 + 0), and a heavy N(0 + 0). Diagonalisation then yields the correct experimental neutrino mass M ∼ (MW2/MN) ∼ eV for MN ∼ 1023 eV.

In both the see-saw and the Yukawa coupling models, all particle masses are generated by the interactions of the particle’s field with the vacuum state. Particles are slowed by vacuum interactions. According to special relativity, slowness is in turn related to the perceived mass. Slowness rises with mass. So massless particles have the least slowness. This does not mean that massless particles, like the photon and probably the graviton, are impervious to the vacuum. E.g. the photons vacuum numbers are not zero, but rather c2=1/(ε 0μ0).

The vacuum also provides a measurable difference between classical and quantum mechanics. John Bell found that difference. In articulating his famous inequality 50 years ago, he said: “For me, it is so reasonable to assume that the photons in those experiments carry with them programs, which have been correlated in advance, telling them how to behave. This is so rational that I think that when Einstein saw that, and the others refused to see it, he was the rational man. … for me, it is a pity that Einstein’s idea doesn’t work. The reasonable thing just doesn’t work.” It is clear that Bell thought and hoped hidden variables would be the answer. But they were not, and the present interpretation is that quantum mechanics requires an observer to put particles on their mass shells.

Neutrinos as probes

Neutrinos’ low mass and neutral charge mean they interact exceedingly weakly with other particles and fields. This feature of weak interaction is of interest particularly 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 mid-20th 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 40,000 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.

Solar neutrinos originate from the nuclear fusion powering the Sun and other stars. The details of the operation of the Sun are explained by Bahcall’s 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 (i.e. 6.5 x 1010) solar neutrinos pass through every square centimetre on the part of the Earth orthogonal to the direction of the Sun. Since neutrinos are insignificantly absorbed by the mass of the Earth, the surface area on the side of the Earth opposite the Sun receives about the same number of neutrinos as the side facing the Sun.

Dark matter

Neutrinos can play an important role in the evolution of the Universe, modifying some of the cosmological observables. It is thought that, just like the cosmic microwave background radiation left over from the Big Bang, there is a background of low-energy neutrinos in our Universe. In the 1980s 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, however.

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. From cosmological measurements, it has been calculated that the sum of the three neutrino masses must be less than one millionth that of the electron. The relic background neutrinos are estimated to have a density of 56 of each type per cubic centimetre and temperature 1.9 K (or 1.7 x 10−4 eV) if they are massless, much colder if their mass exceeds 0.001 eV. Although their density is quite high, relic neutrinos 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 six orders of magnitude.

In 1966, Colgate and White calculated that neutrinos carry away most of the gravitational energy released by the collapse of massive stars, events now categorised as Type Ib and Ic and Type II supernovae. When such stars collapse, matter densities at the core become so high (1017 kg/m3) that the degeneracy of electrons is not enough to prevent protons and electrons from combining to form a neutron and an electron neutrino. A second and more profuse neutrino source is the thermal energy (100 billion kelvins) of the newly formed neutron core, which is dissipated via the formation of neutrino-antineutrino pairs of all flavours. 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. Consequently, supernovae are known to release approximately 99% of their radiant energy in a short (10 second) burst of neutrinos. These neutrinos are a very useful probe for core collapse studies. For an average supernova, approximately 1057 (an octodecillion) neutrinos are released, but the actual number detected at a terrestrial detector will be far smaller; e.g., a dozen neutrinos observed by the Kamiokande II experiment came from Supernova 1987A, which occurred in the Large Magellanic Cloud, a small galaxy that orbits the Milky Way.

Neutrinos are also useful for probing astrophysical other 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. Ultra-high-energy cosmic rays, in the form of swift protons and atomic nuclei, are unable to travel more than about 100 megaparsecs due to the GreisenZatsepin-Kuzmin limit (GZK cut off). Neutrinos, in contrast, can travel even greater distances barely attenuated. The exception are Zettavolt neutrinos which would annihilate resonantly on the relic-neutrino background to produce a ‘Weiler-burst’ of SM particles.

IceCube

In 1987, Francis Halzen came out with the idea of ‘ice-fishing’ cosmic neutrinos. In July 2018, the IceCube neutrino observatory announced that they had traced an extremely-high-energy neutrino that hit their Antarctica-based research station in September 2017 back to its point of origin in the blazar TXS 0506+056 located 3.7 billion light-years away in the direction of the constellation Orion. 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. Very recently, IceCube detected Glashow’s resonant scattering of electron antineutrinos on electrons, opening a new window to study astrophysical sources and particle physics.

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Fig 2. Cutcosky diagram for neutrino oscillation

Several topics in neutrino physics were not included in this report due to brevity concerns. These include the Jarlskog invariant for CP violation in the leptonic sector, the possibility of extra space dimensions with membrane-bulk resonances of neutrinos, or even no space itself through spin networks of neutrinos, the conflict between quantum mechanics and general relativity, black holes and holography, and more on neutrinos as possible dark matter. Some of these topics are quite speculative, but all point to the opportunities for research provided by the simple neutrino.

References

  1. T. J. Weiler,’ Resonant absorption of cosmic ray neutrinos by the relic neutrino background’, Phys. Rev. Lett. 49, 234 (1982)  doi:10.1103/PhysRevLett.49.234
  2. V. D. Barger, S. Pakvasa, T. J. Weiler and K. Whisnant, ‘Bimaximal mixing of three neutrinos’, Phys. Lett. B 437, 107-116 (1998)  doi:10.1016/S0370-2693(98)00880-6
  3. A. Kusenko and T. J. Weiler, ‘Neutrino cross-sections at high-energies and the future observations of ultrahigh-energy cosmic rays’, Phys. Rev. Lett. 88, 161101 (2002)  doi:10.1103/PhysRevLett.88.161101
  4. L. A. Anchordoqui, H. Goldberg, F. Halzen and T. J. Weiler, ‘Galactic point sources of TeV antineutrinos’, Phys. Lett. B 593, 42 (2004)  doi:10.1016/j.physletb.2004.04.054
  5. L. A. Anchordoqui, H. Goldberg, F. Halzen and T. J. Weiler, ‘Neutrinos as a diagnostic of high energy astrophysical processes’, Phys. Lett. B 621, 18-21 (2005) doi:10.1016/j.physletb.2005.06.056
  6. L. A. Anchordoqui, V. Barger, I. Cholis, H. Goldberg, D. Hooper, A. Kusenko, J. G. Learned, D. Marfatia, S. Pakvasa T. C. Paul, and T. J. Weiler, ‘Cosmic Neutrino Pevatrons: A brand new pathway to astronomy, astrophysics, and particle physics’,  JHEAp 1-2, 1-30 (2014)  doi:10.1016/j.jheap.2014.01.001

Please note, this article will also appear in the sixth edition of our quarterly publication.


Contributor Details

Thomas Weiler

Professor
Vanderbilt University
Website: Visit Website

Luis Anchordoqui

Professor
City University of New York
Website: Visit Website

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