View source for Dirac equation

A relativistic wave equation that plays a fundamental role in relativistic quantum mechanics and in quantum field theory. It is used for describing particles with spin $ \dfrac{1}{2} $ (in $ \hbar $ units), for example, electrons, neutrinos, muons, protons, neutrons, etc., positrons and all other corresponding anti-particles, and hypothetical sub-particles such as quarks. The Dirac equation is the foundation of the theory of particles with half-integral spin ($ \dfrac{1}{2} $, $ \dfrac{3}{2} $, $ \dfrac{5}{2} $, etc.), i.e., fermions that obey the Fermi statistics. Thus, the '''Rarita–Schwinger equation''' is a generalization of the Dirac equation for particles with spin $ \dfrac{3}{2} $.

The Dirac equation is a system of four linear homogeneous partial differential equations of the first order with constant complex coefficients that is invariant with respect to the general Lorentz group of transformations:
$$
\gamma^{\alpha} \frac{\partial \psi}{\partial x^{\alpha}} - \mu \psi = 0, \qquad \alpha \in \{ 0,1,2,3 \},
$$
where
* $ \mu \stackrel{\text{df}}{=} \dfrac{m c}{\hbar} $;
* $ m $ is the rest mass;
* $ x = (x^{0},x^{1},x^{2},x^{3}) \in \mathbb{R}^{4} $ with the pseudo-Euclidean metric $ (x,y) \stackrel{\text{df}}{=} \eta_{\alpha \beta} x^{\alpha} y^{\beta} $;
* $ [\eta_{\alpha \beta}] \stackrel{\text{df}}{=} \begin{bmatrix} 1 & 0 & 0 & 0 \\ 0 & -1 & 0 & 0 \\ 0 & 0 & -1 & 0 \\ 0 & 0 & 0 & -1 \end{bmatrix} $ is the metric tensor of Minkowski space with signature $ + 2 $;
* $ \psi $ is the [[Dirac spinor|Dirac spinor]] (bi-spinor), i.e., $ \psi = \begin{bmatrix} \psi_{1} \\ \psi_{2} \\ \psi_{3} \\ \psi_{4} \end{bmatrix} $; and
* $ \gamma^{\alpha} = \gamma^{0},\gamma^{1},\gamma^{2},\gamma^{3} $ are the [[Dirac matrices|Dirac matrices]], which satisfy the relations $ \gamma^{\alpha} \gamma^{\beta} + \gamma^{\beta} \gamma^{\alpha} = 2 \eta^{\alpha \beta} \mathsf{I}_{4} $.

Under the transformations of the variables from the general Lorentz group $ x'^{\alpha} = L_{\mu}^{\alpha} x^{\mu} $ ([[#References|[2]]]), the bi-spinor $ \psi $ transforms in accordance with the formula $ \psi'(x') = S(L) \psi(x) $, where $ S(L) $ is a non-singular complex $ (4 \times 4) $-matrix. The matrices $ S(L) $ form a special two-valued representation of the group $ L $ (where $ S_{\gamma}^{-1} S = L_{\mu}^{\nu} \gamma^{\mu} $). The Dirac equation does not change its form with respect to the new variables $ \psi'(x'^{\alpha}) $ (this is known as '''relativistic invariance'''):
$$
\gamma^{\alpha} \frac{\partial \psi'}{\partial x'^{\alpha}} - \mu \psi' = 0.
$$

The case $ \mu = 0 $ yields the so called '''Weyl equation''', which describes the neutrino. Here, the Dirac equation is subdivided into two independent equations for spinor functions (known as the '''van der Waerden spinors''') $ \phi \stackrel{\text{df}}{=} (\psi_{1},\psi_{2}) $ and $ \chi \stackrel{\text{df}}{=} (\psi_{3},\psi_{4}) $. None of them will be invariant with respect to reflections (a theory in which parity is not preserved).

Any solution of the Dirac equation satisfies the [[Klein–Gordon equation|'''Klein–Gordon equation''']], which describes spin-less scalar particles:
$$
\eta^{\alpha \beta} \frac{\partial^{2} \psi}{\partial x^{\alpha} \partial x^{\beta}} + \mu^{2} \psi = 0, \qquad \alpha,\beta \in \{ 0,1,2,3 \}.
$$
However, not every solution of this equation satisfies the Dirac equation, which is obtained by factorizing the Klein–Gordon equation.

It follows from the Dirac equation that electrons have an intrinsic angular momentum (spin) of $ \dfrac{\hbar}{2} $. The Dirac equation is a complete description (nearly complete, actually — see the article on [[Quantum field theory|quantum field theory]]) of the motion of atomic electrons in the field of the nucleus and in other electromagnetic fields, and also of the interaction of an electron with certain elementary particles.

Any relativistically invariant equation can be represented in the form of the Dirac equation:
$$
\Gamma^{\alpha} \frac{\partial \psi}{\partial x^{\alpha}} - \mu \psi = 0,
$$
where $ \Gamma^{\alpha} $ is a generalization of $ \gamma^{\alpha} $. In the Klein–Gordon equation, the function $ \psi $ has five components, while $ \Gamma^{\alpha} $ are four five-row matrices (known as the '''Duffin-Kemmer matrices''') that satisfy the relations
$$
\Gamma_{\mu} \Gamma_{\nu} \Gamma_{\rho} + \Gamma_{\rho} \Gamma_{\nu} \Gamma_{\mu} = \eta_{\mu \nu} \Gamma_{\rho} + \eta_{\rho \nu} \Gamma_{\mu}, \qquad \Gamma_{\alpha} = \eta_{\alpha \beta} \Gamma^{\beta}.
$$

The interaction of fermions with an electromagnetic field is allowed for by exchanging the derivative $ \dfrac{\partial}{\partial x^{\alpha}} $ for the compensating derivative $ \dfrac{\partial}{\partial x^{\alpha}} - i A_{\alpha} $ (where $ A_{\alpha} $ is the $ 4 $-potential of the electromagnetic field). In the interaction of fermions with a general gauge field ([[Yang–Mills field|Yang–Mills field]]), the compensating derivative is $ \dfrac{\partial}{\partial x^{\alpha}} - A_{\alpha}^{m} \mathsf{I}_{m} $ (where $ A_{\alpha}^{m} $ are the $ 4 $-potentials of the field, and the $ \mathsf{I}_{m} $’s form a basis of the Lie algebra, i.e., are generators of the Lie group). In a similar manner, allowance for the interactions of fermions with the gravitational field, in accordance with the general theory of relativity, results in the generalization of the Dirac equation to a pseudo-Riemannian space-time, by introducing a corresponding compensating (covariant) derivative ([[#References|[3]]]):
$$
\gamma^{\alpha} \! \left( \frac{\partial}{\partial x^{\alpha}} - C_{\alpha} \right) \! \psi - \mu \psi = 0,
$$
where the $ C_{\alpha} $’s are spinor connection coefficients (initially defined with the aid of the tetrad formalism) that satisfy the relations
$$
\frac{\partial \gamma_{\beta}}{\partial x_{\alpha}} - \Gamma_{\alpha \beta}^{\rho} \gamma_{\rho} + \gamma_{\beta} C_{\alpha} - C_{\alpha} \gamma_{\beta} = 0,
$$
or
$$
C_{\alpha} = \frac{1}{4} \gamma^{\sigma} (\Gamma_{\alpha \sigma}^{\rho} \gamma_{\rho} - \partial_{\alpha} \gamma_{\sigma}),
$$
where the $ \Gamma_{\alpha \beta}^{\rho} $’s are Christoffel symbols. The general relativistic generalization of the Dirac equation is indispensable in the study of gravitational collapse, in the description of the predicted effect of particle generation in strong gravitational fields, etc.

In a space with torsion, the Dirac equation includes a non-linear increment of cubic type ([[#References|[4]]]), and it becomes the non-linear equation
$$
\gamma^{\alpha} \! \left( \frac{\partial}{\partial x^{\alpha}} - C_{\alpha} \right) \! \psi - l^{2} \! \left( \overline{\psi} \gamma \gamma^{\beta} \psi \right) \! \gamma \gamma_{\beta} \psi - \mu \psi = 0,
$$
where $ \gamma \stackrel{\text{df}}{=} i \gamma_{5} $, $ l \stackrel{\text{df}}{=} \sqrt{\dfrac{3 \pi G \hbar}{c^{3}}} $, and $ G $ is the gravitation constant.

By analogy, in a non-metric [[Space-time|space-time]] (or Weyl space-time), the Dirac equation also includes a non-linear increment of cubic type ([[#References|[5]]]):
$$
\gamma^{\alpha} \! \left( \frac{\partial}{\partial x^{\alpha}} - C_{\alpha} \right) \! \psi + l^{2} \! \left( \overline{\psi} \gamma^{\alpha} \psi \right) \! \gamma_{\alpha} \psi - \mu \psi = 0,
$$
where $ l \stackrel{\text{df}}{=} \sqrt{\dfrac{4 \pi G \hbar}{3 c^{3}}} $.

The Dirac equation was introduced in 1928 by P.A.M. Dirac.

====References====

<table>
<TR><TD valign="top">[1]</TD><TD valign="top">
P.A.M. Dirac, “The principles of quantum mechanics”, Clarendon Press (1947). {{ZBL|0030.04801}}</TD></TR>
<TR><TD valign="top">[2]</TD><TD valign="top">
N.N. Bogolyubov, D.V. Shirkov, “Introduction to the theory of quantized fields”, Interscience (1959). (Translated from Russian)</TD></TR>
<TR><TD valign="top">[3]</TD><TD valign="top">
D.R. Brill, J.A. Wheeler, “Neutrinos in the gravitational field”, ''Rev. Modern Physics'', '''29''' (1957), pp. 465.</TD></TR>
<TR><TD valign="top">[4]</TD><TD valign="top">
V.I. Rodichev, “The spinor field in space-time with torsion”, ''Zh. Eksper. Teor. Fiz.'', '''40''' (1969), pp. 1469. (In Russian)</TD></TR>
<TR><TD valign="top">[5]</TD><TD valign="top">
V.G. Krechet, “The spinor field and nonmetricity of space-time”, ''Izv. Voozov. Fiz.'', '''6''' (1980), pp. 52. (In Russian)</TD></TR>
<TR><TD valign="top">[6]</TD> <TD valign="top">
J.D. Bjorken, “Relativistic quantum theory”, '''1''', McGraw-Hill (1964).</TD></TR>
</table>

====References====

<table>
<TR><TD valign="top">[a1]</TD><TD valign="top">
H. Umezawa, “Quantum field theory”, North-Holland (1956).</TD></TR>
<TR><TD valign="top">[a2]</TD> <TD valign="top">
Y. Takahashi, “An introduction to field quantization”, Pergamon (1969).</TD></TR>
<TR><TD valign="top">[a3]</TD> <TD valign="top">
R. Roman, “Theory of elementary particles”, North-Holland (1960).</TD></TR>
<TR><TD valign="top">[a4]</TD> <TD valign="top">
V.S. Varadarajan, “Geometry of quantum theory”, '''1–2''', v. Nostrand (1968). (Translated from Russian)</TD></TR>
<TR><TD valign="top">[a5]</TD> <TD valign="top">
S.W. Hawking, G.F.R. Ellis, “The large scale structure of spacetime”, Cambridge Univ. Press (1973).</TD></TR>
</table>