The method is based on the following fact (see for example [1])
If the electromagnetic field F_{ab} satisfies Maxwell's equations
\begin{equation*}
\nabla_{[a}F_{bc]}= 0 \quad\text{and}\quad \nabla^a F_{ab} =0
\end{equation*}
then the Einstein equations are satisfied as well: \begin{equation*} R_{\mu\nu} - \frac{1}{2} R g_{\mu\nu} = 8 \pi T_{\mu\nu} \end{equation*}
A spinor \psi satisfying equation \eqref{eq:20161115b} is called a Killing spinor.
Definitions and conventions about the formulae above can be found at the bottom of this post.
and there is a spinor \psi such that
\begin{equation}\label{eq:20161115b}
(\nabla_{\mu} + i \sqrt{4 \pi} \not F \gamma_{\mu} ) \psi = 0
\end{equation}
and i \bar \psi \gamma^{\mu} \psi is time-like
then the Einstein equations are satisfied as well: \begin{equation*} R_{\mu\nu} - \frac{1}{2} R g_{\mu\nu} = 8 \pi T_{\mu\nu} \end{equation*}
I take the following ansatz for the metric and electromagnetic field of an extreme black hole \begin{align*} ds^2 &= - f(x)^2 dt^2 + g(x)^2 ( dx_1^2 + dx_2^2 + dx_3^2)\\ A_{\mu} dx^{\mu} &= \frac{1}{\sqrt{4 \pi}} h(x) dt, \quad\text{with}\quad F = dA \end{align*}
The functions f(x), g(x) and h(x) do not depend on t. Although all calculations can be easily performed on a computer
after choosing explicit gamma matrices, it gives more insight to work by hand.
I take the following dual tetrad:
\theta^t = f(x) dt and \theta^i = g(x) dx^i. The components of the connection are then
\begin{align*}
\Gamma_{tti}&= \frac{1}{f g}\partial_i f\\
\Gamma_{ijk}&= \frac{1}{g^2} \left( - \delta_{ij} \partial_k g + \delta_{ik} \partial_j g\right)
\end{align*}
thus
\begin{equation*}
\not\Gamma_t = -\frac{1}{2} \frac{1}{f g}\partial_i f\ \gamma^{ti} \\
\end{equation*}
and
\begin{equation*}
\not\Gamma_i = \frac{1}{2} \frac{1}{g^2} \partial_k g\ \gamma^{ik}
\end{equation*}
also
\begin{equation*}
F = \frac{1}{\sqrt{4 \pi}} \partial_i h \ dx^i dt = \frac{1}{\sqrt{4 \pi}} \partial_i h \ g^{-1} f^{-1}\ \theta^i \theta^t
\end{equation*}
thus
\begin{equation*}
\not F = \frac{2}{4} \frac{1}{\sqrt{4 \pi}} \partial_i h \ g^{-1} f^{-1} \gamma^{it}
\end{equation*}
The \mu = t component of equation \eqref{eq:20161115b} then gives
\begin{equation*}
\left[ -\frac{1}{2} \frac{1}{fg} \partial_i f \ \gamma^{ti} + \frac{i}{2} \partial_i h \ g^{-1} f^{-1} \gamma^{it} \gamma_t \right]\psi = 0
\end{equation*}
A solution of this equation is given by h=f and \psi satisfying i \gamma_t \psi = - \psi.
The \mu = i component of equation \eqref{eq:20161115b} gives
\begin{equation*}
\left[e_i +\frac{1}{2} \frac{1}{g^2} \partial_k g\ \gamma^{ik}+ \frac{i}{2} \partial_k h \ g^{-1} f^{-1} \gamma^{kt} \gamma_i \right]\psi = 0
\end{equation*}
Using i \gamma_t \psi = - \psi, this equation is equivalent with
\begin{equation*}
\left[e_i +\frac{1}{2} \frac{1}{g^2} \partial_k g\ \gamma^{ik} - \frac{1}{2} \partial_i h \ g^{-1} f^{-1} - \frac{1}{2} \partial_k h \ g^{-1} f^{-1} \gamma^{ki} \right]\psi = 0
\end{equation*}
This is solved by
e_i(\psi) -\dfrac{1}{2} \partial_i h \ g^{-1} f^{-1}\psi =0 and \dfrac{1}{2} \dfrac{1}{g^2} \partial_k\ g + \dfrac{1}{2} \partial_k h \ g^{-1} f^{-1}=0.
Thus g = f^{-1}. Writing \psi = k(x) \epsilon, with \epsilon a constant spinor, we find k = f ^{1/2}.
Finally, the Maxwell equation \dfrac{1}{\sqrt{-g}} \partial_{\mu} (\sqrt{-g} F^{\mu\nu} ) =0 gives \partial_i ( f^{-2} \partial_i f) =0, thus f^{-1} is
a harmonic function.
All in all, if U(x_1,x_2,x_3) is a harmonic function, then f = U^{-1}, g = U, h = U^{-1} is a solution of the Einstein-Maxwell equations with Killing spinor \psi = U^{-1/2} \epsilon where i \gamma_0 \epsilon = - \epsilon. The special case U(x_1,x_2,x_3) = 1+ \frac{m}{r} with r^2 = x_1^2 + x_2^2 + x_3^3 is the Reissner–Nordström solution with mass equal to the charge. The case with general U is called the Majumdar-Papapetrou solution. Notice that the equations we solved above were all linear. This is much easier than solving the non-linear Einstein equations.
Further reading
This method is related to supersymmetry. The equation \eqref{eq:20161115b} expresses that the supersymmetry variation of the gravitino is zero, and therefore that the solution is supersymmetric. The method can also be generalized to higher dimensions. For example, in [2], the authors classified all supersymmetric solution of (some version of) the five-dimensional Einstein-Maxwell equations. They based their classification on an equation analogous to \eqref{eq:20161115b}.
References
- Black hole solutions in string theory, Maeda and Nozawa, 2011. hep-th/1104.1849
- All supersymmetric solutions of minimal supergravity in five dimensions, Gauntlett, Gutowski, Hull, Pakis and Reall, 2002. hep-th/0209114
Definitions and conventions
- \gamma^a are the gamma matrices that satisfy \{ \gamma^a, \gamma^b\} = 2 \eta^{ab} with \eta^{ab}=\text{diagonal}(-1,1,1,1)
- \gamma^{ab} = \frac{1}{2} (\gamma^a \gamma^b - \gamma^b \gamma^a)
-
The covariant derivative of a spinor is
\begin{equation*}
(\nabla_{\mu} \psi)^{\alpha} = \partial_{\mu} \psi^{\alpha} + \Gamma^{\alpha}_{\mu\beta} \psi^{\beta}
\end{equation*}with \Gamma^{\alpha}_{\mu\beta} = - \frac{1}{4} \Gamma_{\mu ab} (\gamma^{ab})^{\alpha}_{\ \ \beta}.
- \Gamma_{\mu ab} are the components of the spin connection where \omega^a_{\ \ b} = \Gamma^a_{\mu b} dx^{\mu} and \Gamma_{\mu ab} = \eta{bc}\Gamma^c_{\mu a}.
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