Sterile neutrinos (or inert neutrinos) are hypothetical particles[1] (neutral leptons – neutrinos) that interact only via gravity and do not interact via any of the fundamental interactions of the Standard Model. The term sterile neutrino is used to distinguish them from the known active neutrinos in the Standard Model, which carry an isospin charge of ±+1/2 under the weak interaction.
This term usually refers to neutrinos with right-handed chirality (see right-handed neutrino), which may be added to the Standard Model. Occasionally it is used in a general sense for any neutral fermion, instead of the more cautiously vague name neutral heavy leptons (NHLs) or heavy neutral leptons (HNLs).
The existence of right-handed neutrinos is theoretically well-motivated, since all other known fermions have been observed with both left and right chirality, and since they could explain in a natural way the small active neutrino masses inferred from neutrino oscillation. The mass of the right-handed neutrinos themselves is unknown and could have any value between 1015 GeV and less than 1 eV.[2]
The number of sterile neutrino types (if they exist) is not yet constrained by theory. This is in contrast to the number of active neutrino types, which has to equal that of charged leptons and quark generations to ensure the electroweak interaction is free of anomalies.
The search for sterile neutrinos is an active area of particle physics. If they exist and their mass is smaller than the energies of particles in the experiment, they can be produced in the laboratory, either by mixing between active and sterile neutrinos or in high energy particle collisions. If they are heavier, the only directly observable consequence of their existence would be the observed active neutrino masses. They may, however, be responsible for a number of unexplained phenomena in physical cosmology and astrophysics, including dark matter, baryogenesis or dark radiation.[2] In May 2018, physicists of the MiniBooNE experiment reported a stronger neutrino oscillation signal than expected, a possible hint of sterile neutrinos.[3][4]
Motivation
See also: Neutrino: Chirality and Neutrino oscillation
Experimental results show that all produced and observed neutrinos have left-handed helicities (spin antiparallel to momentum), and all antineutrinos have right-handed helicities, within the margin of error. In the massless limit, it means that only one of two possible chiralities is observed for either particle. These are the only helicities (and chiralities) included in the Standard Model of particle interactions.
Recent experiments such as neutrino oscillation, however, have shown that neutrinos have a non-zero mass, which is not predicted by the Standard Model and suggests new, unknown physics. This unexpected mass explains neutrinos with right-handed helicity and antineutrinos with left-handed helicity: Since they do not move at the speed of light, their helicity is not relativistic invariant (it is possible to move faster than them and observe the opposite helicity). Yet all neutrinos have been observed with left-handed chirality, and all antineutrinos right-handed. Chirality is a fundamental property of particles and is relativisticly invariant: It is the same regardless of the particle's speed and mass in every inertial reference frame. However, a particle with mass that starts out with left-handed chirality can develop a right-handed component as it travels – unless it is massless, chirality is not conserved during the propagation of a free particle through space.
The question, thus, remains: Do neutrinos and antineutrinos differ only in their chirality? Or do exotic right-handed neutrinos and left-handed antineutrinos exist as separate particles from the common left-handed neutrinos and right-handed antineutrinos?
Properties
Such particles would belong to a singlet representation with respect to the strong interaction and the weak interaction, having zero electric charge, zero weak hypercharge, zero weak isospin, and, as with the other leptons, zero color charge, although they do have a B − L quantum number of −1. If the standard model is embedded in a hypothetical SO(10) grand unified theory, they can be assigned an X charge of −5. The left-handed anti-neutrino has a B − L of +1 and an X charge of +5.
Due to the lack of electric charge, hypercharge, and color charge, sterile neutrinos would not interact electromagnetically, weakly, or strongly, making them extremely difficult to detect. They have Yukawa interactions with ordinary leptons and Higgs bosons, which via the Higgs mechanism leads to mixing with ordinary neutrinos.
In experiments involving energies larger than their mass, sterile neutrinos would participate in all processes in which ordinary neutrinos take part, but with a quantum mechanical probability that is suppressed by a small mixing angle. That makes it possible to produce them in experiments, if they are light enough to be within the reach of current particle accelerators.
They would also interact gravitationally due to their mass, and if they are heavy enough, could explain cold dark matter or warm dark matter. In some grand unification theories, such as SO(10), they also interact via gauge interactions which are extremely suppressed at ordinary energies because their gauge boson is extremely massive. They do not appear at all in some other GUTs, such as the Georgi–Glashow model ( i.e., all its SU(5) charges or quantum numbers are zero).
Mass
All particles are initially massless under the Standard Model, since there are no Dirac mass terms in the Standard Model's Lagrangian. The only mass terms are generated by the Higgs mechanism, which produces non-zero Yukawa couplings between the left-handed components of fermions, the Higgs field, and their right-handed components. This occurs when the SU(2) doublet Higgs field \( \phi \) acquires its non-zero vacuum expectation value, \( \nu \), spontaneously breaking its SU(2)L × U(1) symmetry, and thus yielding non-zero Yukawa couplings:
\( {\displaystyle {\mathcal {L}}(\psi )={\bar {\psi }}(i\partial \!\!\!/)\psi -G{\bar {\psi }}_{L}\phi \psi _{R}} \)
Such is the case for charged leptons, like the electron, but within the standard model the right-handed neutrino does not exist. So absent the sterile right chiral neutrinos to pair up with the left chiral neutrinos, even with Yukawa coupling the active neutrinos remain massless. In other words, there are no mass-generating terms for neutrinos under the Standard Model: For each generation, the model only contains a left-handed neutrino and its antiparticle, a right-handed antineutrino, each of which is produced in weak eigenstates during weak interactions; the "sterile" neutrinos are omitted. (See neutrino masses in the Standard Model for a detailed explanation.)
In the seesaw mechanism, the model is extended to include the missing right-handed neutrinos and left-handed antineutrinos; one of the eigenvectors of the neutrino mass matrix is then hypothesized to be remarkably heavier than the other.
A sterile (right-chiral) neutrino would have the same weak hypercharge, weak isospin, and electric charge as its antiparticle, because all of these are zero and hence are unaffected by sign reversal.[a]
Dirac and Majorana terms
Sterile neutrinos allow the introduction of a Dirac mass term as usual. This can yield the observed neutrino mass, but it requires that the strength of the Yukawa coupling be much weaker for the electron neutrino than the electron, without explanation. Similar problems (although less severe) are observed in the quark sector, where the top and bottom masses differ by a factor of 40.
Unlike for the left-handed neutrino, a Majorana mass term can be added for a sterile neutrino without violating local symmetries (weak isospin and weak hypercharge) since it has no weak charge. However, this would still violate total lepton number.
It is possible to include both Dirac and Majorana terms: this is done in the seesaw mechanism (below). In addition to satisfying the Majorana equation, if the neutrino were also its own antiparticle, then it would be the first Majorana fermion. In that case, it could annihilate with another neutrino, allowing neutrinoless double beta decay. The other case is that it is a Dirac fermion, which is not its own antiparticle.
To put this in mathematical terms, we have to make use of the transformation properties of particles. For free fields, a Majorana field is defined as an eigenstate of charge conjugation. However, neutrinos interact only via the weak interactions, which are not invariant under charge conjugation (C), so an interacting Majorana neutrino cannot be an eigenstate of C. The generalized definition is: "a Majorana neutrino field is an eigenstate of the CP transformation". Consequently, Majorana and Dirac neutrinos would behave differently under CP transformations (actually Lorentz and CPT transformations). Also, a massive Dirac neutrino would have nonzero magnetic and electric dipole moments, whereas a Majorana neutrino would not. However, the Majorana and Dirac neutrinos are different only if their rest mass is not zero. For Dirac neutrinos, the dipole moments are proportional to mass and would vanish for a massless particle. Both Majorana and Dirac mass terms however can appear in the mass Lagrangian.
Seesaw mechanism
Main article: Seesaw mechanism
In addition to the left-handed neutrino, which couples to its family charged lepton in weak charged currents, if there is also a right-handed sterile neutrino partner (a weak isosinglet with zero charge) then it is possible to add a Majorana mass term without violating electroweak symmetry. Both neutrinos have mass and handedness is no longer preserved (thus "left or right-handed neutrino" means that the state is mostly left or right-handed). To get the neutrino mass eigenstates, we have to diagonalize the general mass matrix \( {\displaystyle M_{\nu }} \):
\( {\displaystyle M_{\nu }={\begin{pmatrix}0&m_{D}\\m_{D}&M_{NHL}\end{pmatrix}}} \)
where \( M_{{NHL}} \) is big and \( m_{D} \) is of intermediate size terms.
Apart from empirical evidence, there is also a theoretical justification for the seesaw mechanism in various extensions to the Standard Model. Both Grand Unification Theories (GUTs) and left-right symmetrical models predict the following relation:
\( {\displaystyle m_{\nu }\ll m_{D}\ll M_{NHL}} \)
According to GUTs and left-right models, the right-handed neutrino is extremely heavy: \( {\textstyle M_{NHL}\approx } \) 105 to 1012 GeV, while the smaller eigenvalue is approximately equal to
\( m_{{\nu }}\approx {\frac {m_{D}^{2}}{M_{{NHL}}}} \)
This is the seesaw mechanism: as the sterile right-handed neutrino gets heavier, the normal left-handed neutrino gets lighter. The left-handed neutrino is a mixture of two Majorana neutrinos, and this mixing process is how sterile neutrino mass is generated.
Detection attempts
The production and decay of sterile neutrinos could happen through the mixing with virtual ("off mass shell") neutrinos. There were several experiments set up to discover or observe NHLs, for example the NuTeV (E815) experiment at Fermilab or LEP-l3 at CERN. They all led to establishing limits to observation, rather than actual observation of those particles. If they are indeed a constituent of dark matter, sensitive X-ray detectors would be needed to observe the radiation emitted by their decays.[5]
Sterile neutrinos may mix with ordinary neutrinos via a Dirac mass after electroweak symmetry breaking, in analogy to quarks and charged leptons. Sterile neutrinos and (in more-complicated models) ordinary neutrinos may also have Majorana masses. In the type 1 seesaw mechanism both Dirac and Majorana masses are used to drive ordinary neutrino masses down and make the sterile neutrinos much heavier than the Standard Model's interacting neutrinos. In some models the heavy neutrinos can be as heavy as the GUT scale (≈1015 GeV). In other models[which?] they could be lighter than the weak gauge bosons W and Z as in the so-called νMSM model where their masses are between GeV and keV. A light (with the mass ≈1 eV) sterile neutrino was suggested as a possible explanation of the results of the Liquid Scintillator Neutrino Detector experiment. On 11 April 2007, researchers at the MiniBooNE experiment at Fermilab announced that they had not found any evidence supporting the existence of such a sterile neutrino.[6] More-recent results and analysis have provided some support for the existence of the sterile neutrino.[7][8]
Two separate detectors near a nuclear reactor in France found 3% of anti-neutrinos missing. They suggested the existence of a fourth neutrino with a mass of 1.2 eV.[9] Sterile neutrinos are also candidates for dark radiation. Daya Bay has also searched for a light sterile neutrino and excluded some mass regions.[10] Daya Bay Collaboration measured the anti-neutrino energy spectrum, and found that anti-neutrinos at an energy of around 5 MeV are in excess relative to theoretical expectations. It also recorded 6% missing anti-neutrinos.[11] This could suggest either that sterile neutrinos exist or that our understanding of some other aspect of neutrinos is incomplete.
The number of neutrinos and the masses of the particles can have large-scale effects that shape the appearance of the cosmic microwave background. The total number of neutrino species, for instance, affects the rate at which the cosmos expanded in its earliest epochs: More neutrinos means a faster expansion. The Planck Satellite 2013 data release is compatible with the existence of a sterile neutrino. The implied mass range is from 0–3 eV.[12][failed verification – see discussion] In 2016, scientists at the IceCube Neutrino Observatory did not find any evidence for the sterile neutrino.[13] However, in May 2018, physicists of the MiniBooNE experiment reported a stronger neutrino oscillation signal than expected, a possible hint of sterile neutrinos.[3][4]
See also
MiniBooNE at Fermilab
Footnotes
And as with all other particle / anti-particle pairs, the sterile right-chiral neutrino and left-chiral anti-neutrino would also have identical, non-zero mass. Chirality, lepton-number, and flavor (if any) are the only quantum numbers that distinguish a sterile neutrino from a sterile antineutrino. For any charged particle, for example the electron, this is not the case: Its antiparticle, the positron, has opposite electric charge, opposite weak isospin, and opposite chirality, among other opposite charges. Similarly, an up quark has a charge of ++2/3 and, for example, a color charge of red, while its antiparticle has an electric charge of −+2/3 and in this example a color charge of anti-red.
References
"A major physics experiment just detected a particle that shouldn't exist". Live Science. NBC News. 2018.
Drewes, Marco (2013). "The phenomenology of right handed neutrinos". International Journal of Modern Physics E. 22 (8): 1330019–593. arXiv:1303.6912. Bibcode:2013IJMPE..2230019D. doi:10.1142/S0218301313300191.
Letzter, Rafi (1 June 2018). "A major physics experiment just detected a particle that shouldn't exist". LiveScience. Retrieved 3 June 2018.
Collaboration, MiniBooNE; Aguilar-Arevalo, A.A.; Brown, B.C.; Bugel, L.; Cheng, G.; Conrad, J.M.; et al. (2018). "Observation of a significant excess of electron-like events in the MiniBooNE short-baseline neutrino experiment". Physical Review Letters. 121 (22): 221801. arXiv:1805.12028. Bibcode:2018PhRvL.121v1801A. doi:10.1103/PhysRevLett.121.221801. PMID 30547637.
Battison, Leila (16 September 2011). "Dwarf galaxies suggest dark matter theory may be wrong". BBC News. Retrieved 18 September 2011.
"First results" (PDF). Booster Neutrino Experiment (BooNE). Fermi National Accelerator Laboratory (Fermilab).
"Dimensional shortcuts" . Scientific American. August 2007.
Bulbul, E.; Markevitch, M.; Foster, A.; Smith, R.K.; Loewenstein, M.; Randall, S.W. (2014). "Detection of an unidentified emission line in the stacked X-ray spectrum of galaxy clusters". The Astrophysical Journal. 789 (1): 13.arXiv:1402.2301. Bibcode:2014ApJ...789...13B. doi:10.1088/0004-637X/789/1/13.
"The reactor antineutrino anomaly". irfu.cea.fr.
An, F. P.; Balantekin, A. B.; Band, H. R.; Beriguete, W.; Bishai, M.; Blyth, S.; et al. (1 October 2014). "Search for a light sterile neutrino at Daya Bay". Physical Review Letters. 113 (14): 141802.arXiv:1407.7259. Bibcode:2014PhRvL.113n1802A. doi:10.1103/PhysRevLett.113.141802. PMID 25325631.
"Daya Bay discovers a mismatch". Symmetry.
Ade, P.A.R.; et al. (Planck Collaboration) (2013). "Planck 2013 results. XVI. Cosmological parameters". Astronomy and Astrophysics. 571: A16. arXiv:1303.5076. Bibcode:2014A&A...571A..16P. doi:10.1051/0004-6361/201321591.
"Icy telescope throws cold water on sterile neutrino theory". Nature. 8 August 2016. Retrieved 12 August 2016.
Drewes, M. (2013). "The phenomenology of right handed neutrinos". International Journal of Modern Physics E. 22 (8): 1330019. arXiv:1303.6912. Bibcode:2013IJMPE..2230019D. doi:10.1142/S0218301313300191.
Merle, A. (2013). "keV neutrino model building". International Journal of Modern Physics D. 22 (10): 1330020.arXiv:1302.2625. Bibcode:2013IJMPD..2230020M. doi:10.1142/S0218271813300206.
Vaitaitis, A. G.; et al. (1999). "Search for Neutral Heavy Leptons in a High-Energy Neutrino Beam". Physical Review Letters. 83 (24): 4943–4946.arXiv:hep-ex/9908011. Bibcode:1999PhRvL..83.4943V. doi:10.1103/PhysRevLett.83.4943.
Formaggio, J.A.; Conrad, J.; Shaevitz, M.; Vaitaitis, A. (1998). "Helicity effects in neutral heavy lepton decays". Physical Review D. 57 (11): 7037–7040. Bibcode:1998PhRvD..57.7037F. doi:10.1103/PhysRevD.57.7037.
Nakamura, K.; Particle Data Group (2010). "Review of Particle Physics". Journal of Physics G. 37 (75021): 075021. Bibcode:2010JPhG...37g5021N. doi:10.1088/0954-3899/37/7A/075021.
Dark matter
Forms of
dark matter
Baryonic dark matter Cold dark matter Hot dark matter Light dark matter Mixed dark matter Warm dark matter Self-interacting dark matter Scalar field dark matter Primordial black holes
Hypothetical particles
Axino Axion Dark photon Holeum LSP Minicharged particle Neutralino Sterile neutrino SIMP WIMP
Theories
and objects
Cuspy halo problem Dark fluid Dark galaxy Dark globular cluster Dark matter halo Dark radiation Dark star Dwarf galaxy problem Halo mass function Mass dimension one fermions Massive compact halo object Mirror matter Navarro–Frenk–White profile Scalar field dark matter
Search
experiments
Direct
detection
ADMX ANAIS ArDM CDEX CDMS CLEAN CoGeNT COSINE COUPP CRESST CUORE D3 DAMA/LIBRA DAMA/NaI DAMIC DarkSide DARWIN DEAP DM-Ice DMTPC DRIFT EDELWEISS EURECA KIMS LUX LZ MACRO MIMAC NAIAD NEWAGE NEWS-G PandaX PICASSO PICO ROSEBUD SABRE SIMPLE TREX-DM UKDMC WARP XENON XMASS ZEPLIN
Indirect
detection
AMS-02 ANTARES ATIC CALET CAST DAMPE Fermi HAWC HESS IceCube MAGIC MOA OGLE PAMELA VERITAS
Other projects
Potential dark galaxies
HE0450-2958 HVC 127-41-330 Smith's Cloud VIRGOHI21
Related
Antimatter Dark energy Exotic matter Galaxy formation and evolution Illustris project Imaginary mass Negative mass UniverseMachine
Hellenica World - Scientific Library
Retrieved from "http://en.wikipedia.org/"
All text is available under the terms of the GNU Free Documentation License
