fields and particles in particle physics
and in the standard model of particle physics:
matter field fermions (spinors, Dirac fields)
flavors of fundamental fermions in the standard model of particle physics: | |||
---|---|---|---|
generation of fermions | 1st generation | 2nd generation | 3d generation |
quarks ($q$) | |||
up-type | up quark ($u$) | charm quark ($c$) | top quark ($t$) |
down-type | down quark ($d$) | strange quark ($s$) | bottom quark ($b$) |
leptons | |||
charged | electron | muon | tauon |
neutral | electron neutrino | muon neutrino | tau neutrino |
bound states: | |||
mesons | light mesons: pion ($u d$) ρ-meson ($u d$) ω-meson ($u d$) f1-meson a1-meson | strange-mesons: ϕ-meson ($s \bar s$), kaon, K*-meson ($u s$, $d s$) eta-meson ($u u + d d + s s$) charmed heavy mesons: D-meson ($u c$, $d c$, $s c$) J/ψ-meson ($c \bar c$) | bottom heavy mesons: B-meson ($q b$) ϒ-meson ($b \bar b$) |
baryons | nucleons: proton $(u u d)$ neutron $(u d d)$ |
(also: antiparticles)
hadrons (bound states of the above quarks)
minimally extended supersymmetric standard model
bosinos:
dark matter candidates
Exotica
The axion is a hypothetical type of field/fundamental particle originally hypothesized (Weinberg 77, Wilczek 78) as a solution to the strong CP problem in the standard model of particle physics. After the initial model for the axion was quickly ruled out by experiment (see Wilczek 78 for the early history) a variant model was found (Dine-Fischler-Srednicki 81), called the “invisible axion”, which does not violate experimental bounds.
The “invisible axion” turns out to also be a natural candidate for dark matter Preskill-Wise-Wilczek 83, hence potentially also solves one of the problems with the standard model of cosmology. More recently it is argued in Hui-Ostriker-Tremaine-Witten 16 that indeed axionic dark matter (fuzzy dark matter) potentially solves the remaining problems of standard WIMP dark matter models: WIMP dark matter models work exceedingly well on cosmological scales but has serious experimental problems on the scale of galaxies. Due to the extreme lightness of axion particles, their de Broglie wavelength may be of the scale of galaxies and hence their quantum properties may become relevant at this scale to deviate in the right way from the WIMP models.
The Pecchei-Quinn shift symmetry of the axion and the peculiar nature of the axion interaction term which are needed to make the axion model work this way have been argued to naturally arise in string theory, if the axion is identified with the KK-reduction of the higher gauge fields in string theory. This we discuss below.
The problem here is that the action functional for QCD (Yang-Mills theory) a priori contains an arbitrary theta angle $\theta$
but that – since the term $tr(F_\nabla \wedge F_\nabla)$ causes parity violation, which is strongly constrained by experiment – there must be some reason why $\theta$ vanishes or else is extremely small.
(Here the term $tr(F_\nabla \wedge F_\nabla)$ is the invariant polynomial for the second Chern class, measuring the instanton number of the gauge field $\nabla$.)
The solution to this problem via axions is to assume that $\theta$ is not really a fundamental parameter, but instead is the vacuum expectation value of a dynamical field $a$ (the axion).
The idea is that a standard kinetic action
together with the axion interaction term
makes $a$ have vanishing expectation value $\langle a\rangle$. This would give a dynamical explanation why under the identification of the theta angle with this expectation value
the theta angle vanishes.
That this is indeed the case is due to Vafa-Witten 84, around (2). These authors argue via the Wick rotated path integral as follows:
Under Wick rotation, parity-violating terms in the Lagrangian density pick up an imaginary factor $i$. Therefore the path integral expression for the Wick rotated vacuum energy is
Now due to the factor of $i$ in front of $\theta$ in this expression, the real part of the argument of the logarithm necessarily becomes smaller with $a$. Therefore the negative logarithm becomes larger with $a$. Accordingly $E_{vac}(a)$ must have a minimum at $\theta = 0$ (according to Vafa-Witten 84, p.2).
In string theory axion fields
are naturally present as the KK-reduction of the higher gauge fields (e.g. Svrcek-Witten 06);
reviewed below in:
are generically of positive but tiny mass (ADDKM 09, Acharya-Bobkov-Kumar 10) as they need to be to be a solution to the strong CP problem and be candidates for BEC/superfluid/fuzzy dark matter;
reviewed below in:
This makes axion fields in string theory form a curious confluence point relating
with
In string theory axion fields naturally arise as the KK compactification of the higher gauge fields (B-field, C-field, RR-fields). Here we review how this comes about.
Notice that this means that axions in string theory are as in the output of the original Peccei–Quinn proposal, but do not actually make use of the Peccei–Quinn mechanism.
As amplified in particular in Svrcek-Witten 06:
An obvious question about the axion hypothesis is how natural it really is. Why introduce a global PQ “symmetry” if it is not actually a symmetry? What is the sense in constraining a theory so that the classical Lagrangian possesses a certain symmetry if the symmetry is actually anomalous? It could be argued that the best evidence that PQ “symmetries” are natural comes from string theory, which produces them without any contrivance. … the string compactifications always generate PQ symmetries, often spontaneously broken at the string scale and producing axions, but sometimes unbroken. (Svrcek-Witten 06, pages 3-4)
Similarly from ADDKM 09:
However, at the effective field theory level it is hard to judge how natural it is to have such a “fake” global PQ symmetry which is explicitly broken exclusively by QCD. Note, that in order not to spoil the solution to the strong CP problem all other sources of explicit PQ symmetry breaking should be at least 10 orders of magnitude down with respect to the potential generated by the QCD anomaly, and one may be especially cautious about the viability of such a proposal, given the common lore that global symmetries always get broken by quantum gravitational effects [12, 13, 14]. This makes it natural to inquire whether axions arise naturally in the most developed quantum theory of gravity—string theory. (ADDKM 09, p. 3)
The mechanism discussed in Svrcek-Witten 06, in all its incarnations in the various perspectives on string theory (heterotic strings, type II strings, 11-dimensional supergravity with M-theory effects included, etc.) share the following properties:
the axion field itself is the double dimensional reduction of one of the higher gauge fields in string theory, the (twisted) Kalb-Ramond field for heterotic string, the RR-field for the type II string, or the supergravity C-field in 11-dimensional supergravity with M-brane effects;
accordingly the Peccei-Quinn periodic shift symmetry of the axion results arises as the $U(1)$-gauge symmetry that is the dimensional reduction of the $B^2 U(1)$ (heterotic B-field) or $B^3 U(1)$ (11d C-field) higher gauge symmetry, where the $U(1)$-periodicity is ultimately due to the higher Dirac charge quantization for these fields;
the axion interaction term of the form $\propto a \langle F \wedge F\rangle$ arises as the double dimensional reduction of the self-interaction terms of these higher gauge fields:
in type II string theory it is a component of the higher WZW term on coincident D6-branes with a component $\propto A_{3}^{RR} \wedge \langle F \wedge F\rangle$,
for 11d C-fields it is the term $\propto C_{3} \wedge \langle F \wedge F\rangle$ induced by anomaly cancellation for M-theory at conical singularities (as discussed at M-theory on G₂-manifolds)
for heterotic string theory it arises from integrating out the Lagrange multiplier that enforces the Green-Schwarz anomaly cancellation in 4d.
We now discuss this in more detail:
Consider string phenomenology in type IIA string theory in the guise of intersecting D-brane models with the standard model of particle physics supported in intersecting D6-branes whose worldvolume fills all of 4d spacetime.
The higher WZW term in the Green-Schwarz action functional for the D6-brane is of the form
where $A^RR$ denotes the collective inhomogenous background RR-field and $F_\nabla$ is the curvature 2-form of the Chan-Paton gauge field on the D-brane. The $\langle -\rangle$ denotes the Killing form invariant polynomial, hence the trace for the special unitary Lie algebra regarded as a matrix Lie algebra. $X_7$ denotes the worldvolume of the D6-brane
Hence one of the three non-vanishing summands in this expression is
Now assuming a Kaluza-Klein ansatz $X_7 = X_4 \times Y_3$ with
the effective axion field in 4d, then this term becomes the axion interaction term
(Svrcek-Witten 06, around (6.9))
In heterotic string theory KK-compactified to 4d, the 4d B-field, dualized, serves as the axion field, called the “model independent axion” (Svrcek-Witten 06, starting p. 15).
This works as follows: By the Green-Schwarz anomaly cancellation mechanism, then B-field in heterotic string theory is a twisted 2-form field, whose field strength $H$ locally has in addition to the exact differential $d B$ also a fundamental 3-form contribution, so that
(locally). Moreover, the differential $d H$ is constrained to be the Pontryagin 4-form of the gauge potential $\nabla$ (minus that of the Riemann curvature, but let’s suppress this notationally for the present purpose):
Now suppose KK-compactification to 4d has been taken care of, then this constraint may be implemented in the equations of motion by adding it to the action functional, multiplied with a Lagrange multiplier :
Now by the usual argument, one says that instead of varying by $a$ and thus implementing the Green-Schwarz anomaly cancellation constraint, it is equivalent to first vary with respect to the other fields, and then insert the resulting equations in terms of $a$ into the action functional.
Now since we are dealing with a twisted B-field, with free 3-form component $C$, we actually vary with respect to $C$. This yields the Euler-Lagrange equation of motion
hence the usual relation or electro-magnetic duality, expressing what used to be the Lagrange multiplier now as the magentic dual field to the twisted B-field.
Plugging this algebraic equation of motion back into the above action functional for $H$ gives
This now is an action functional for an axion field $a$ of just the form required above for the solution of the strong CP-problem.
From Acharya-Kane-Kumar 12, p. 3:
Now consider the axions. Due to the shift symmetries mentioned above, there are no perturbative contributions to their potential. Non-perturbative effects though, such as strong gauge dynamics, gauge instantons, gaugino condensation and stringy instantons will generate a potential for the axions. Because any such contribution is exponentially suppressed by couplings and/or extra-dimensional volumes, in our world with perturbative gauge couplings (at high scales), the axion masses will be exponentially small.
Furthermore, since there are large numbers of axions in general, their masses will essentially be uniformly distributed on a logarithmic scale (5). See (6) for a detailed calculation of axion masses in string/M effective theories.
Like the moduli, the axions are also very weakly coupled to matter and therefore do not thermalize in general. Moreover, since their masses are tiny - ranging from $m_{3/2}$ to even below the Hubble scale today - many of them, including the QCD axion, start coherent oscillations during the time that the moduli are dominating the energy density, but before BBN.
Observe that ultralight axion fields is precisely what is required in HEP phenomenology for
the solution to the strong CP-problem;
the solution of the dark matter problem via BEC/superfluid/wave/fuzzy dark matter (e.g. Hui-Ostriker-Tremaine-Witten 16).
The axion as such was originally proposed in
Steven Weinberg, New light boson, Phys. Rev. Lett. 40:223-6 (1977)
Frank Wilczek, Problem of strong P and T invariance in the presence of instantons, Phys. Rev. Lett. 40:279-82 (1978)
The experimentally viable variant as the “invisible axion” is due to
The observation that the “invisible axion” is a candidate for dark matter is due to three groups:
John Preskill, M. Wise, Frank Wilczek, Cosmology of the invisible axion, Phys. Lett. B 120:127-32 (1983)
L.F. Abbott, P. Sikivie, A Cosmological Bound on the Invisible Axion, Phys.Lett. B120:133-36 (1983)
Michael Dine, Willy Fischler, The Not So Harmless Axion, Phys. Lett. B120 :137-141 (1983)
A historical recollection of the development until here is in
The argument that the topological interaction term $\propto a \langle F \wedge F\rangle$ gives the axion field $a$ a vanishing vacuum expectation value is due to
A reformulation of this effect in terms of Chern-Simons forms is discussed in
Review:
Markus Kuster, Georg Raffelt, Berta Beltrán (eds.), Axions: Theory, cosmology, and Experimental Searches, Lect. Notes Phys. 741 (Springer, Berlin Heidelberg 2008) (doi:10.1007/978-3-540-73518-2_2)
Jihn E. Kim, Gianpaolo Carosi, Axions and the Strong CP Problem, Rev.Mod.Phys.82:557-602,2010 (arXiv:0807.3125)
Masahiro Kawasaki, Kazunori Nakayama, Axions : Theory and Cosmological Role, Annual Review of Nuclear and Particle Science Vol.63:1-552 (arXiv:1301.1123)
Luca Di Luzio, Maurizio Giannotti, Enrico Nardi, Luca Visinelli, The landscape of QCD axion models (arXiv:2003.01100)
Igor G. Irastorza, An introduction to axions and their detection (arXiv:2109.07376)
See also:
Discussion of the various ways that axions naturally appear in string theory is in
Specifically for the F-theory sector of string theory:
Specifically open string axions
A textbook account of axion string phenomenology is in
Discussion of stringy axion cosmology (such as fuzzy dark matter) is in
Asimina Arvanitaki, Savas Dimopoulos, Sergei Dubovsky, Nemanja Kaloper, John March-Russell, String Axiverse, Phys.Rev.D81:123530,2010 (arXiv:0905.4720)
Bobby Acharya, Konstantin Bobkov, Piyush Kumar, An M Theory Solution to the Strong CP Problem and Constraints on the Axiverse, JHEP 1011:105, 2010 (arXiv:1004.5138)
Bobby Acharya, Gordon Kane, Piyush Kumar, Compactified String Theories – Generic Predictions for Particle Physics, Int. J. Mod. Phys. A, Volume 27 (2012) 1230012 (arXiv:1204.2795)
Realization in the Witten-Sakai-SUgimoto model? for holographic QCD:
Discussion of experimental signatures of and constraints on axion physics:
Discussion of experimental signatures of and constraints on axion physics from particle physics:
Specifically contribution of axions to the anomalous magnetic moment of the electron and muon in QED:
Yannis Semertzidis, Magnetic and Electric Dipole Moments in Storage Rings, chapter 6 of Markus Kuster, Georg Raffelt, Berta Beltrán (eds.), Axions: Theory, cosmology, and Experimental Searches, Lect. Notes Phys. 741 (Springer, Berlin Heidelberg 2008) (Kuster-Raffelt-Beltran 08, doi:10.1007/978-3-540-73518-2_2)
Roberta Armillis, Claudio Coriano’, Marco Guzzi, Simone Morelli, Axions and Anomaly-Mediated Interactions: The Green-Schwarz and Wess-Zumino Vertices at Higher Orders and g-2 of the muon, JHEP 0810:034,2008 (arXiv:0808.1882)
W.J. Marciano, A. Masiero, P. Paradisi, M. Passera, Contributions of axion-like particles to lepton dipole moments, Phys. Rev. D 94, 115033 (2016) (arXiv:1607.01022)
Martin Bauer, Matthias Neubert, Andrea Thamm, Collider Probes of Axion-Like Particles, J. High Energ. Phys. (2017) 2017: 44. (arXiv:1708.00443, doi:10.1007/JHEP12(2017)044)
The basic relevant Feynman diagrams are worked out here:
See also
For the ABRACADABRA (A Broadband/Resonant Approach to Cosmic Axion Detection with an Amplifying B-field Ring Apparatus) approach to axion detection, see
For the ADMX experiment:
Axion signatures in gravitational waves potentially visible by LIGO-type experiments are discussed in
Discussion of experimental signatures of and constraints on axion physics in cosmology, where the axion is a (fuzzy) dark matter-candidate:
Joseph P. Conlon, M.C. David Marsh, Searching for a 0.1-1 keV Cosmic Axion Background (arXiv:1305.3603)
Primordial decays of string theory moduli at $z \sim 10^{12}$ naturally generate a dark radiation Cosmic Axion Background (CAB) with $0.1 - 1 keV$ energies. This CAB can be detected through axion-photon conversion in astrophysical magnetic fields to give quasi-thermal excesses in the extreme ultraviolet and soft X-ray bands. Substantial and observable luminosities may be generated even for axion-photon couplings $\ll 10^{-11} GeV^{-1}$. We propose that axion-photon conversion may explain the observed excess emission of soft X-rays from galaxy clusters, and may also contribute to the diffuse unresolved cosmic X-ray background. We list a number of correlated predictions of the scenario.
Discussion of the axion as a candidate for dark matter (fuzzy dark matter) is in
with its experimental bounds
and as a candidate for dark energy:
Last revised on July 18, 2024 at 11:31:55. See the history of this page for a list of all contributions to it.