Relativistic wave equations
In physics, specifically relativistic quantum mechanics (RQM) and its applications to particle physics, relativistic wave equations predict the behavior of particles at high energies and velocities comparable to the speed of light. In the context of quantum field theory (QFT), the equations determine the dynamics of quantum fields.
The solutions to the equations, universally denoted as ψ or Ψ (Greek psi), are referred to as "wave functions" in the context of RQM, and "fields" in the context of QFT. The equations themselves are called "wave equations" or "field equations", because they have the mathematical form of a wave equation or are generated from a Lagrangian density and the fieldtheoretic Euler–Lagrange equations (see classical field theory for background).
In the Schrödinger picture, the wave function or field is the solution to the Schrödinger equation;
one of the postulates of quantum mechanics. All relativistic wave equations can be constructed by specifying various forms of the Hamiltonian operator Ĥ describing the quantum system. Alternatively, Feynman's path integral formulation uses a Lagrangian rather than a Hamiltonian operator.
More generally – the modern formalism behind relativistic wave equations is Lorentz group theory, wherein the spin of the particle has a correspondence with the representations of the Lorentz group.^{[1]}
HistoryEdit
Early 1920s: Classical and quantum mechanicsEdit
The failure of classical mechanics applied to molecular, atomic, and nuclear systems and smaller induced the need for a new mechanics: quantum mechanics. The mathematical formulation was led by De Broglie, Bohr, Schrödinger, Pauli, and Heisenberg, and others, around the mid1920s, and at that time was analogous to that of classical mechanics. The Schrödinger equation and the Heisenberg picture resemble the classical equations of motion in the limit of large quantum numbers and as the reduced Planck constant ħ, the quantum of action, tends to zero. This is the correspondence principle. At this point, special relativity was not fully combined with quantum mechanics, so the Schrödinger and Heisenberg formulations, as originally proposed, could not be used in situations where the particles travel near the speed of light, or when the number of each type of particle changes (this happens in real particle interactions; the numerous forms of particle decays, annihilation, matter creation, pair production, and so on).
Late 1920s: Relativistic quantum mechanics of spin0 and spin1/2 particlesEdit
A description of quantum mechanical systems which could account for relativistic effects was sought for by many theoretical physicists; from the late 1920s to the mid1940s.^{[2]} The first basis for relativistic quantum mechanics, i.e. special relativity applied with quantum mechanics together, was found by all those who discovered what is frequently called the Klein–Gordon equation:

(1)
by inserting the energy operator and momentum operator into the relativistic energy–momentum relation:

(2)
The solutions to (1) are scalar fields. The KG equation is undesirable due to its prediction of negative energies and probabilities, as a result of the quadratic nature of (2) – inevitable in a relativistic theory. This equation was initially proposed by Schrödinger, and he discarded it for such reasons, only to realize a few months later that its nonrelativistic limit (what is now called the Schrödinger equation) was still of importance. Nevertheless, – (1) is applicable to spin0 bosons.^{[3]}
Neither the nonrelativistic nor relativistic equations found by Schrödinger could predict the fine structure in the Hydrogen spectral series. The mysterious underlying property was spin. The first twodimensional spin matrices (better known as the Pauli matrices) were introduced by Pauli in the Pauli equation; the Schrödinger equation with a nonrelativistic Hamiltonian including an extra term for particles in magnetic fields, but this was phenomenological. Weyl found a relativistic equation in terms of the Pauli matrices; the Weyl equation, for massless spin1/2 fermions. The problem was resolved by Dirac in the late 1920s, when he furthered the application of equation (2) to the electron – by various manipulations he factorized the equation into the form:

(3A)
and one of these factors is the Dirac equation (see below), upon inserting the energy and momentum operators. For the first time, this introduced new fourdimensional spin matrices α and β in a relativistic wave equation, and explained the fine structure of hydrogen. The solutions to (3A) are multicomponent spinor fields, and each component satisfies (1). A remarkable result of spinor solutions is that half of the components describe a particle while the other half describe an antiparticle; in this case the electron and positron. The Dirac equation is now known to apply for all massive spin1/2 fermions. In the nonrelativistic limit, the Pauli equation is recovered, while the massless case results in the Weyl equation.
Although a landmark in quantum theory, the Dirac equation is only true for spin1/2 fermions, and still predicts negative energy solutions, which caused controversy at the time (in particular – not all physicists were comfortable with the "Dirac sea" of negative energy states).
1930s–1960s: Relativistic quantum mechanics of higherspin particlesEdit
The natural problem became clear: to generalize the Dirac equation to particles with any spin; both fermions and bosons, and in the same equations their antiparticles (possible because of the spinor formalism introduced by Dirac in his equation, and thenrecent developments in spinor calculus by van der Waerden in 1929), and ideally with positive energy solutions.^{[2]}
This was introduced and solved by Majorana in 1932, by a deviated approach to Dirac. Majorana considered one "root" of (3A):

(3B)
where ψ is a spinor field now with infinitely many components, irreducible to a finite number of tensors or spinors, to remove the indeterminacy in sign. The matrices α and β are infinitedimensional matrices, related to infinitesimal Lorentz transformations. He did not demand that each component of 3B to satisfy equation (2), instead he regenerated the equation using a Lorentzinvariant action, via the principle of least action, and application of Lorentz group theory.^{[4]}^{[5]}
Majorana produced other important contributions that were unpublished, including wave equations of various dimensions (5, 6, and 16). They were anticipated later (in a more involved way) by de Broglie (1934), and Duffin, Kemmer, and Petiau (around 1938–1939) see Duffin–Kemmer–Petiau algebra. The Dirac–Fierz–Pauli formalism was more sophisticated than Majorana’s, as spinors were new mathematical tools in the early twentieth century, although Majorana’s paper of 1932 was difficult to fully understand; it took Pauli and Wigner some time to understand it, around 1940.^{[2]}
Dirac in 1936, and Fierz and Pauli in 1939, built equations from irreducible spinors A and B, symmetric in all indices, for a massive particle of spin n + ½ for integer n (see Van der Waerden notation for the meaning of the dotted indices):

(4A)

(4B)
where p is the momentum as a covariant spinor operator. For n = 0, the equations reduce to the coupled Dirac equations and A and B together transform as the original Dirac spinor. Eliminating either A or B shows that A and B each fulfill (1).^{[2]}
In 1941, Rarita and Schwinger focussed on spin^{3}⁄_{2} particles and derived the Rarita–Schwinger equation, including a Lagrangian to generate it, and later generalized the equations analogous to spin n + ½ for integer n. In 1945, Pauli suggested Majorana's 1932 paper to Bhabha, who returned to the general ideas introduced by Majorana in 1932. Bhabha and Lubanski proposed a completely general set of equations by replacing the mass terms in (3A) and (3B) by an arbitrary constant, subject to a set of conditions which the wave functions must obey.^{[6]}
Finally, in the year 1948 (the same year as Feynman's path integral formulation was cast), Bargmann and Wigner formulated the general equation for massive particles which could have any spin, by considering the Dirac equation with a totally symmetric finitecomponent spinor, and using Lorentz group theory (as Majorana did): the Bargmann–Wigner equations.^{[2]}^{[7]} In the early 1960s, a reformulation of the Bargmann–Wigner equations was made by H. Joos and Steven Weinberg, the Joos–Weinberg equation. Various theorists at this time did further research in relativistic Hamiltonians for higher spin particles.^{[1]}^{[8]}^{[9]}
1960s–presentEdit
The relativistic description of spin particles has been a difficult problem in quantum theory. It is still an area of the presentday research because the problem is only partially solved; including interactions in the equations is problematic, and paradoxical predictions (even from the Dirac equation) are still present.^{[5]}
Linear equationsEdit
The following equations have solutions which satisfy the superposition principle, that is, the wave functions are additive.
Throughout, the standard conventions of tensor index notation and Feynman slash notation are used, including Greek indices which take the values 1, 2, 3 for the spatial components and 0 for the timelike component of the indexed quantities. The wave functions are denoted ψ, and ∂_{μ} are the components of the fourgradient operator.
In matrix equations, the Pauli matrices are denoted by σ^{μ} in which μ = 0, 1, 2, 3, where σ^{0} is the 2 × 2 identity matrix:
and the other matrices have their usual representations. The expression
is a 2 × 2 matrix operator which acts on 2component spinor fields.
The gamma matrices are denoted by γ^{μ}, in which again μ = 0, 1, 2, 3, and there are a number of representations to select from. The matrix γ^{0} is not necessarily the 4 × 4 identity matrix. The expression
is a 4 × 4 matrix operator which acts on 4component spinor fields.
Note that terms such as "mc" scalar multiply an identity matrix of the relevant dimension, the common sizes are 2 × 2 or 4 × 4, and are conventionally not written for simplicity.
Particle spin quantum number s Name Equation Typical particles the equation describes 0 Klein–Gordon equation Massless or massive spin0 particle (such as Higgs bosons). 1/2 Weyl equation Massless spin1/2 particles. Dirac equation Massive spin1/2 particles (such as electrons). Twobody Dirac equations Massive spin1/2 particles (such as electrons). Majorana equation Massive Majorana particles. Breit equation Two massive spin1/2 particles (such as electrons) interacting electromagnetically to first order in perturbation theory. 1 Maxwell equations (in QED using the Lorenz gauge) Photons, massless spin1 particles. Proca equation Massive spin1 particle (such as W and Z bosons). 3/2 Rarita–Schwinger equation Massive spin3/2 particles. s Bargmann–Wigner equations where ψ is a rank2s 4component spinor.
Free particles of arbitrary spin (bosons and fermions).^{[8]}^{[10]} Joos–Weinberg equation Free particles of arbitrary spin (bosons and fermions).
Linear gauge fieldsEdit
The Duffin–Kemmer–Petiau equation is an alternative equation for spin0 and spin1 particles:
Constructing RWEsEdit
Using 4vectors and the energy–momentum relationEdit
Start with the standard special relativity (SR) 4vectors
Note that each 4vector is related to another by a Lorentz scalar:
 , where is the proper time
 , where is the rest mass
 , which is the 4vector version of the Planck–Einstein relation & the de Broglie matter wave relation
 , which is the 4gradient version of complexvalued plane waves
Now, just apply the standard Lorentz scalar product rule to each one:
The last equation is a fundamental quantum relation.
When applied to a Lorentz scalar field , one gets the Klein–Gordon equation, the most basic of the quantum relativistic wave equations.
 : in 4vector format
 : in tensor format
 : in factored tensor format
The Schrödinger equation is the lowvelocity limiting case (v << c) of the Klein–Gordon equation.
When the relation is applied to a fourvector field instead of a Lorentz scalar field , then one gets the Proca equation (in Lorenz gauge):
If the rest mass term is set to zero (lightlike particles), then this gives the free Maxwell equation (in Lorenz gauge)
Representations of the Lorentz groupEdit
Under a proper orthochronous Lorentz transformation x → Λx in Minkowski space, all oneparticle quantum states ψ^{j}_{σ} of spin j with spin zcomponent σ locally transform under some representation D of the Lorentz group:^{[11]}^{[12]}
where D(Λ) is some finitedimensional representation, i.e. a matrix. Here ψ is thought of as a column vector containing components with the allowed values of σ. The quantum numbers j and σ as well as other labels, continuous or discrete, representing other quantum numbers are suppressed. One value of σ may occur more than once depending on the representation. Representations with several possible values for j are considered below.
The irreducible representations are labeled by a pair of halfintegers or integers (A, B). From these all other representations can be built up using a variety of standard methods, like taking tensor products and direct sums. In particular, spacetime itself constitutes a 4vector representation (1/2, 1/2) so that Λ ∈ D'^{(1/2, 1/2)}. To put this into context; Dirac spinors transform under the (1/2, 0) ⊕ (0, 1/2) representation. In general, the (A, B) representation space has subspaces that under the subgroup of spatial rotations, SO(3), transform irreducibly like objects of spin j, where each allowed value:
occurs exactly once.^{[13]} In general, tensor products of irreducible representations are reducible; they decompose as direct sums of irreducible representations.
The representations D^{(j, 0)} and D^{(0, j)} can each separately represent particles of spin j. A state or quantum field in such a representation would satisfy no field equation except the Klein–Gordon equation.
Nonlinear equationsEdit
There are equations which have solutions that do not satisfy the superposition principle.
Nonlinear gauge fieldsEdit
 Yang–Mills equation: describes a nonabelian gauge field
 Yang–Mills–Higgs equations: describes a nonabelian gauge field coupled with a massive spin0 particle
Spin 2Edit
 Einstein field equations: describe interaction of matter with the gravitational field (massless spin2 field):
 The solution is a metric tensor field, rather than a wave function.
See alsoEdit
ReferencesEdit
NotesEdit
 ^ ^{a} ^{b} T Jaroszewicz; P.S Kurzepa (1992). "Geometry of spacetime propagation of spinning particles". Annals of Physics. Bibcode:1992AnPhy.216..226J. doi:10.1016/00034916(92)90176M.
 ^ ^{a} ^{b} ^{c} ^{d} ^{e} S. Esposito (2011). "Searching for an equation: Dirac, Majorana and the others". Annals of Physics. 327 (6): 1617–1644. arXiv:1110.6878. Bibcode:2012AnPhy.327.1617E. doi:10.1016/j.aop.2012.02.016.
 ^ B. R. Martin, G.Shaw (2008). Particle Physics. Manchester Physics Series (3rd ed.). John Wiley & Sons. p. 3. ISBN 9780470032947.
 ^ R. Casalbuoni (2006). "Majorana and the Infinite Component Wave Equations". Pos Emc. 2006: 004. arXiv:hepth/0610252.
 ^ ^{a} ^{b} X. Bekaert; M.R. Traubenberg; M. Valenzuela (2009). "An infinite supermultiplet of massive higherspin fields". Journal of High Energy Physics. 2009 (5): 118. arXiv:0904.2533. Bibcode:2009JHEP...05..118B. doi:10.1088/11266708/2009/05/118.
 ^ R.K. Loide; I. Ots; R. Saar (1997). "Bhabha relativistic wave equations". Journal of Physics A: Mathematical and General. 30 (11): 4005–4017. Bibcode:1997JPhA...30.4005L. doi:10.1088/03054470/30/11/027.
 ^ Bargmann, V.; Wigner, E. P. (1948). "Group theoretical discussion of relativistic wave equations". Proc. Natl. Acad. Sci. U.S.A. 34 (5): 211–23. Bibcode:1948PNAS...34..211B. doi:10.1073/pnas.34.5.211. PMC 1079095. PMID 16578292.
 ^ ^{a} ^{b} E.A. Jeffery (1978). "Component Minimization of the Bargman–Wigner wavefunction". Australian Journal of Physics. 31 (2): 137–149. Bibcode:1978AuJPh..31..137J. doi:10.1071/ph780137.
 ^ R.F Guertin (1974). "Relativistic hamiltonian equations for any spin". Annals of Physics. 88 (2): 504–553. Bibcode:1974AnPhy..88..504G. doi:10.1016/00034916(74)901808.
 ^ R.Clarkson, D.G.C. McKeon (2003). "Quantum Field Theory" (PDF). pp. 61–69. Archived from the original (PDF) on 20090530.
 ^ Weinberg, S. (1964). "Feynman Rules for Any spin" (PDF). Phys. Rev. 133 (5B): B1318–B1332. Bibcode:1964PhRv..133.1318W. doi:10.1103/PhysRev.133.B1318.; Weinberg, S. (1964). "Feynman Rules for Any spin. II. Massless Particles" (PDF). Phys. Rev. 134 (4B): B882–B896. Bibcode:1964PhRv..134..882W. doi:10.1103/PhysRev.134.B882.; Weinberg, S. (1969). "Feynman Rules for Any spin. III" (PDF). Phys. Rev. 181 (5): 1893–1899. Bibcode:1969PhRv..181.1893W. doi:10.1103/PhysRev.181.1893.
 ^ K. Masakatsu (2012). "Superradiance Problem of Bosons and Fermions for Rotating Black Holes in Bargmann–Wigner Formulation". arXiv:1208.0644 [grqc].
 ^ Weinberg, S (2002), "5", The Quantum Theory of Fields, vol I, p. [1], ISBN 0521550017
Further readingEdit
 R.G. Lerner; G.L. Trigg (1991). Encyclopaedia of Physics (2nd ed.). VHC publishers. ISBN 0895737523.
 C.B. Parker (1994). McGraw Hill Encyclopaedia of Physics (2nd ed.). ISBN 0070514003.
 G. Woan, Cambridge University Press (2010). The Cambridge Handbook of Physics Formulas. ISBN 9780521575072.
 D. McMahon (2006). Relativity DeMystified. Mc Graw Hill (USA). ISBN 0071455450.
 J.A. Wheeler; C. Misner; K.S. Thorne (1973). Gravitation. W.H. Freeman. ISBN 0716703440.
 B.R. Martin; G. Shaw (2008). Particle Physics (Manchester series) (2nd ed.). John Wiley & Sons. ISBN 9780470032947.
 P. Labelle, Demystified (2010). Supersymmetry. McGrawHill (USA). ISBN 9780071636414.
 B.H. Bransden; C.J. Joachain (1983). Physics of Atoms and Molecules. Longman. ISBN 0582444012.
 E. Abers (2004). Quantum Mechanics. Addison Wesley. ISBN 9780131461000.
 D. McMahon (2008). Quantum Field Theory. Mc Graw Hill (USA). ISBN 9780071543828.
 M. Pillin (1994). "qDeformed Relativistic Wave Equations". Journal of Mathematical Physics. 35 (6): 2804–2817. arXiv:hepth/9310097. Bibcode:1994JMP....35.2804P. doi:10.1063/1.530487.