The Einstein Field Equations

Contents
  1. The route to the field equations
  2. The stress–energy tensor
  3. The Bianchi identities
  4. The Newtonian correspondence
  5. The linearized theory
  6. The cosmological constant
  7. Lovelock's uniqueness theorem
  8. Energy conditions
  9. The initial-value problem
  10. Exact solutions: an overview

The field equations relate the curvature of spacetime, constructed in Geometric Formulation of Gravity on the mathematical foundation of Differentiable Manifolds, Tensors, and Curvature, to the energy and momentum of matter. This chapter presents them along Einstein's route of November 1915 [Einstein:1915b], derives them in full from the Hilbert action [Hilbert:1915], establishes energy–momentum conservation as a consequence of the Bianchi identities rather than a separate postulate, fixes the coupling constant by Newtonian correspondence, and states, with Lovelock, that in four dimensions the equations are essentially unique [Lovelock:1971].

The remaining sections supply what every later chapter of this part draws on: the cosmological constant [Einstein:1917a], the energy conditions that power the singularity theorems, the initial-value formulation that makes the theory predictive [ChoquetBruhat:1952], and an overview of the exact solutions — Schwarzschild, Kerr, Friedmann–Lemaître–Robertson–Walker — whose detailed study is Schwarzschild Geometry and Black Holes and Evidence-Based Cosmology.

Conventions, fixed once for the whole chapter: the signature is \((-,+,+,+)\) with coordinates \(x^{\mu}=(x^{0},x^{i})=(ct,\vect{x})\), as in Gravitational-Wave Theory and Appendix A.1; the connection is the torsion-free Levi-Civita connection of Theorem 13.150, written \(\Gamma^{\lambda}{}_{\mu\nu}\) without the ring accent of Geometric Formulation of Gravity since no other connection appears; and the curvature conventions are Equation (13.306) and Equation (13.307), for which the round sphere has \(R>0\). The mostly-minus convention of Minkowski Space and Its Symmetries differs by \(g_{\mu\nu}\to-g_{\mu\nu}\); wherever this chapter leans on a result stated in that convention, the statement used is one whose signature bookkeeping is tracked explicitly (the \(\epsilon\) discipline of Appendix A.52), and the substitution made is said in place.

The route to the field equations

Requirements on a relativistic theory of gravity

Newtonian gravity fails relativity twice: the Poisson equation propagates influence instantaneously, and the force law singles out a preferred family of frames. What replaces it cannot be guessed freely; by 1915 the constraints on any candidate were sharp, and it is worth stating them as the specification the field equations must meet, because the rest of this chapter checks them off one by one [Einstein:1916a].

  1. The equivalence principle. Free fall is universal to the accuracy of the Eötvös-class experiments (Phenomenon 42.1), so gravity is not a force field on spacetime but a property of spacetime itself: test bodies follow geodesics of a metric \(g_{\mu\nu}\) (Postulate 43.1), and the field variable of the theory is the metric.

  2. General covariance. The equations must be tensor equations, well formed in every coordinate system, since the equivalence principle deprives any coordinate system of intrinsic meaning (but see the caveat of Remark 44.1).

  3. Newtonian correspondence. For weak, static fields and slow motion the theory must reduce to the inverse-square dynamics of Newtonian Dynamics and Central Forces and Statics, in the field form of the Poisson equation; this is Section 44.4.

  4. Second-order field equations. The equations should contain no derivatives of \(g_{\mu\nu}\) beyond the second, so that the initial-value problem has the shape of every other field theory in this treatise; higher-derivative dynamics generically suffers the Ostrogradsky instability (Proposition 16.39 and Remark 16.40).

  5. A conserved source. The source must be the energy–momentum content of matter, described by a symmetric tensor \(T_{\mu\nu}\) (Section 44.2), and the equations must be compatible with its local conservation — not impose it as an extra axiom.

These five requirements do not merely motivate the Einstein equations; by Lovelock's theorem (Section 44.7) they very nearly force them, up to the two constants \(\kappa\) and \(\Lambda\) fixed in Section 44.4.2 and Section 44.6.

Remark 44.1 (The Kretschmann objection).

General covariance by itself is physically empty: as Kretschmann observed — the argument circulated in 1917, the printed issue is dated 1918 — any theory, Newtonian gravity included, can be rewritten in generally covariant form by carrying enough auxiliary structure along [Kretschmann:1918]. What distinguishes general relativity is not covariance but the absence of prior geometry: the metric is the only spacetime structure, and it is dynamical. The modern assessment of the dispute, and of what Einstein's covariance arguments do and do not establish, is reviewed in [Norton:1993]. Requirement (ii) above is therefore to be read together with this stronger condition: no non-dynamical background fields.

The November 1915 papers

The final theory arrived in four communications to the Prussian Academy, one week apart. On 4 November Einstein abandoned the restricted covariance of the 1913 Entwurf theory — whose troubled trajectory, including the hole argument against general covariance that he first accepted and then dismantled, is traced in [Norton:1993] — and proposed equations covariant under unimodular coordinate transformations [Einstein:1915d]. On 11 November an addendum sharpened the hypothesis on the trace of the source [Einstein:1915e]. On 18 November he applied the vacuum equations — which the later correction would not touch — to the perihelion of Mercury and obtained the observed 43 seconds of arc per century with no adjustable parameter [Einstein:1915a], the computation whose experimental content is Experiment: The Classical Tests of General Relativity. On 25 November the trace term fell into place and the equations took their final, generally covariant form [Einstein:1915b]. The episode is a working example of the methodology of Epistemology and the Scientific Method: two years of false steps constrained by one hard number.

Definition 44.2 (Einstein tensor).

The Einstein tensor of \((M,g)\) is

\begin{equation}\tag{44.1} G_{\mu\nu} = R_{\mu\nu} - \tfrac{1}{2}\,g_{\mu\nu}R\ec \end{equation}

with \(R_{\mu\nu}\) and \(R\) the Ricci contractions of Definition 13.153. It is symmetric, carries SI dimension \(/\mathrm{m}^{2}\), and is divergence-free as an identity (Theorem 44.23). Rests on Definition 13.153.

Postulate 44.3 (Einstein field equations).

The metric of spacetime is determined by the energy–momentum content of matter through

\begin{equation}\tag{44.2} G_{\mu\nu} = \frac{8\pi G}{c^{4}}\,T_{\mu\nu}\ec \end{equation}

with \(T_{\mu\nu}\) the stress–energy tensor of Section 44.2 [Einstein:1915b]. The coupling constant \(\kappa=8\pi G/c^{4}\) is fixed by Newtonian correspondence in Section 44.4.2. Rests on Definition 44.2.

Equation (44.2) is ten coupled, quasilinear, second-order partial differential equations for the ten components of \(g_{\mu\nu}\) — of which only six are independent, by the four contracted Bianchi identities (Remark 44.25). The same physical postulate can be packaged as an action principle, which is the subject of Section 44.1.3; the postulate proper is then the choice of action.

Proposition 44.4 (Trace-reversed form).

Equation (44.2) is equivalent to

\begin{equation}\tag{44.3} R_{\mu\nu} = \kappa\left(T_{\mu\nu}-\tfrac{1}{2}\,g_{\mu\nu}T\right)\ec \qquad T = g^{\alpha\beta}T_{\alpha\beta}\ep \end{equation}

In particular the vacuum equations are \(R_{\mu\nu}=0\): vacuum solutions are Ricci-flat, not flat. Rests on Postulate 44.3.

Proof.

Derives Proposition 44.4. Tracing Equation (44.2) with \(g^{\mu\nu}\) in \(D=4\) gives \(R-2R=\kappa T\), so \(R=-\kappa T\). Substituting back, \(R_{\mu\nu}=\kappa T_{\mu\nu}+\tfrac12 g_{\mu\nu}R =\kappa(T_{\mu\nu}-\tfrac12 g_{\mu\nu}T)\), and the two forms determine each other. With \(T_{\mu\nu}=0\) both give \(R_{\mu\nu}=0\), while the Riemann tensor need not vanish — the Schwarzschild exterior (Section 44.10) is the standing example. This trace-reversed form is the one Einstein printed on 25 November [Einstein:1915b], and it is the form the Newtonian limit reads most easily (Section 44.4.2).

The Hilbert action

Five days before the final field equations, Hilbert presented an action from which they follow by variation [Hilbert:1915]: the Einstein–Hilbert action of Definition 43.2, here instantiated at \(D=4\),

\begin{equation}\tag{44.4} S_{\mathrm{EH}}[g] = \frac{1}{2\kappa}\int_{\Omega}\dd^{4}x\,\sqrt{\abs{g}}\;R\ec \end{equation}

together with a matter action \(S_{\mathrm{m}}[\psi;g]\) for the matter fields \(\psi\). This subsection carries out the variation in full — it is the derivation deferred to this chapter by Remark 43.4 — including the boundary term that the usual compact-support argument hides, and the first-order variation in vielbein-form variables.

Remark 44.5 (SI bookkeeping for the action).

With \(x^{0}=ct\) the measure \(\dd^{4}x\) carries \(\mathrm{m}^{4}\), \(R\) carries \(/\mathrm{m}^{2}\) and \(\kappa=8\pi G/c^{4}\) carries \(\mathrm{s}^{2}/\mathrm{kg}/\mathrm{m}\), so Equation (44.4) carries \(\mathrm{J}\,\mathrm{m}\): it is \(c\) times a conventional action in \(\mathrm{J}\,\mathrm{s}\), because the time coordinate is measured in metres. Extremals are unaffected by the constant factor. The same convention is applied to \(S_{\mathrm{m}}\), so that the tensor defined next comes out in \(\mathrm{J}/\mathrm{m}^{3}\), the SI unit of energy density.

Definition 44.6 (Stress–energy tensor).

Let \(S_{\mathrm{m}}[\psi;g]\) be the action of the matter fields, covariantly coupled to the metric and carrying no other spacetime structure. The stress–energy tensor of the matter is its metric variational derivative,

\begin{equation}\tag{44.5} T_{\mu\nu} := -\frac{2}{\sqrt{\abs{g}}}\, \frac{\delta S_{\mathrm{m}}}{\delta g^{\mu\nu}}\ec \qquad\text{equivalently}\qquad \delta S_{\mathrm{m}} = -\frac{1}{2}\int\dd^{4}x\,\sqrt{\abs{g}}\; T_{\mu\nu}\,\delta g^{\mu\nu}\ec \end{equation}

the functional derivative being the field-theoretic first variation of Theorem 16.36. \(T_{\mu\nu}\) is symmetric by construction, and \(T_{\mu\nu}\) carries \(\mathrm{J}/\mathrm{m}^{3}\): \(T_{00}\) is an energy density, \(cT_{0i}\) an energy flux, \(T_{ij}\) a stress. Rests on Theorem 16.36.

Two variational lemmas do all the work. Both are pure algebra plus one classical determinant identity.

Lemma 44.7 (Variation of inverse and determinant).

Under a variation \(\delta g_{\mu\nu}\) of the metric,

\begin{equation}\tag{44.6} \delta g^{\mu\nu} = -\,g^{\mu\alpha}g^{\nu\beta}\,\delta g_{\alpha\beta}\ec \end{equation}
\begin{equation}\tag{44.7} \delta\sqrt{\abs{g}} = \tfrac{1}{2}\sqrt{\abs{g}}\;g^{\mu\nu}\,\delta g_{\mu\nu} = -\tfrac{1}{2}\sqrt{\abs{g}}\;g_{\mu\nu}\,\delta g^{\mu\nu}\ep \end{equation}

Rests on Proposition 5.2.

Proof.

Derives Lemma 44.7. Varying \(g^{\mu\alpha}g_{\alpha\nu}=\delta^{\mu}_{\nu}\) gives \(\delta g^{\mu\alpha}\,g_{\alpha\nu} =-g^{\mu\alpha}\,\delta g_{\alpha\nu}\); contracting with \(g^{\nu\beta}\) yields Equation (44.6). For the determinant, Jacobi's formula Equation (5.21) applied to the matrix \(g_{\mu\nu}\) along any one-parameter family gives \(\delta(\det g)=(\det g)\,g^{\mu\nu}\delta g_{\mu\nu}\), and since \(\abs{g}=-\det g\) here, \(\delta\sqrt{\abs{g}} =\tfrac12\abs{g}^{-1/2}\,\delta\abs{g} =\tfrac12\sqrt{\abs{g}}\,g^{\mu\nu}\delta g_{\mu\nu}\). The second equality in Equation (44.7) follows from Equation (44.6).

Lemma 44.8 (Palatini identity).

The variation of the Levi-Civita connection is the tensor

\begin{equation}\tag{44.8} \delta\Gamma^{\lambda}{}_{\mu\nu} = \tfrac{1}{2}g^{\lambda\rho}\left( \nabla_{\mu}\delta g_{\rho\nu} + \nabla_{\nu}\delta g_{\rho\mu} - \nabla_{\rho}\delta g_{\mu\nu}\right)\ec \end{equation}

and the variation of the Ricci tensor is its covariant curl,

\begin{equation}\tag{44.9} \delta R_{\mu\nu} = \nabla_{\lambda}\,\delta\Gamma^{\lambda}{}_{\nu\mu} - \nabla_{\nu}\,\delta\Gamma^{\lambda}{}_{\lambda\mu}\ep \end{equation}

Consequently the trace is a pure divergence,

\begin{equation}\tag{44.10} g^{\mu\nu}\,\delta R_{\mu\nu} = \nabla_{\mu}v^{\mu}\ec\qquad v^{\mu} = g^{\alpha\beta}\,\delta\Gamma^{\mu}{}_{\alpha\beta} - g^{\mu\beta}\,\delta\Gamma^{\lambda}{}_{\lambda\beta}\ec \end{equation}

with, explicitly in terms of the metric variation,

\begin{equation}\tag{44.11} v^{\mu} = g^{\mu\rho}g^{\alpha\beta} \left(\nabla_{\alpha}\delta g_{\rho\beta} - \nabla_{\rho}\delta g_{\alpha\beta}\right)\ep \end{equation}

Rests on Theorem 13.150, Theorem 13.152 and Definition 13.149.

Proof.

Derives Lemma 44.8. Step 1: Equation (44.8). Vary the Christoffel formula of Theorem 13.150, \(\Gamma^{\lambda}{}_{\mu\nu}=\tfrac12 g^{\lambda\rho} (\pp_{\mu}g_{\rho\nu}+\pp_{\nu}g_{\rho\mu}-\pp_{\rho}g_{\mu\nu})\). The \(\delta g^{\lambda\rho}\) term contributes, by Equation (44.6) and the same formula read backwards, \(-g^{\lambda\alpha}\,\Gamma^{\sigma}{}_{\mu\nu}\,\delta g_{\alpha\sigma}\). In the \(\delta(\pp g)\) terms replace each \(\pp\,\delta g\) by \(\nabla\,\delta g\) plus its two connection terms; summing the three combinations, four of the six connection terms cancel in pairs by the symmetry of \(\Gamma\), and the surviving two give \(+g^{\lambda\rho}\,\Gamma^{\sigma}{}_{\mu\nu}\,\delta g_{\rho\sigma}\), which cancels the \(\delta g^{\lambda\rho}\) contribution exactly. What remains is Equation (44.8); being built covariantly from the tensor \(\delta g_{\mu\nu}\), it is a tensor — as the difference of two connections must be.

Step 2: Equation (44.9). Vary Equation (13.306):

\begin{equation*} \delta R^{\lambda}{}_{\rho\mu\nu} = \pp_{\mu}\delta\Gamma^{\lambda}{}_{\nu\rho} - \pp_{\nu}\delta\Gamma^{\lambda}{}_{\mu\rho} + \delta\Gamma^{\lambda}{}_{\mu\sigma}\Gamma^{\sigma}{}_{\nu\rho} + \Gamma^{\lambda}{}_{\mu\sigma}\delta\Gamma^{\sigma}{}_{\nu\rho} - \delta\Gamma^{\lambda}{}_{\nu\sigma}\Gamma^{\sigma}{}_{\mu\rho} - \Gamma^{\lambda}{}_{\nu\sigma}\delta\Gamma^{\sigma}{}_{\mu\rho}\ep \end{equation*}

On the other hand, treating \(\delta\Gamma\) as the \((1,2)\) tensor it is,

\begin{equation*} \nabla_{\mu}\delta\Gamma^{\lambda}{}_{\nu\rho} - \nabla_{\nu}\delta\Gamma^{\lambda}{}_{\mu\rho} = \pp_{\mu}\delta\Gamma^{\lambda}{}_{\nu\rho} - \pp_{\nu}\delta\Gamma^{\lambda}{}_{\mu\rho} + \Gamma^{\lambda}{}_{\mu\sigma}\delta\Gamma^{\sigma}{}_{\nu\rho} - \Gamma^{\lambda}{}_{\nu\sigma}\delta\Gamma^{\sigma}{}_{\mu\rho} + \Gamma^{\sigma}{}_{\nu\rho}\delta\Gamma^{\lambda}{}_{\mu\sigma} - \Gamma^{\sigma}{}_{\mu\rho}\delta\Gamma^{\lambda}{}_{\nu\sigma}\ec \end{equation*}

the terms in \(\Gamma^{\sigma}{}_{\mu\nu}\delta\Gamma^{\lambda}{}_{\sigma\rho}\) cancelling between the two covariant derivatives because \(\Gamma^{\sigma}{}_{\mu\nu}\) is symmetric. The right-hand sides agree term by term, so \(\delta R^{\lambda}{}_{\rho\mu\nu} =\nabla_{\mu}\delta\Gamma^{\lambda}{}_{\nu\rho} -\nabla_{\nu}\delta\Gamma^{\lambda}{}_{\mu\rho}\); contracting \(\lambda\) with \(\mu\) gives Equation (44.9).

Step 3: Equation (44.10). Contract Equation (44.9) with \(g^{\mu\nu}\) and pull the metric through \(\nabla\) by metricity (Definition 13.149); the first expression for \(v^{\mu}\) results. Substituting Equation (44.8): in the first slot, \(g^{\alpha\beta}\delta\Gamma^{\mu}{}_{\alpha\beta} =g^{\mu\rho}g^{\alpha\beta}(\nabla_{\alpha}\delta g_{\rho\beta} -\tfrac12\nabla_{\rho}\delta g_{\alpha\beta})\); in the second, \(\delta\Gamma^{\lambda}{}_{\lambda\beta} =\tfrac12 g^{\lambda\rho}\nabla_{\beta}\delta g_{\rho\lambda}\) because the first and third terms of Equation (44.8) cancel under the \(\lambda\rho\) contraction. Combining the two, the half-terms add up and give Equation (44.11).

Theorem 44.9 (Variation of the Einstein–Hilbert action).

For any variation \(\delta g_{\mu\nu}\),

\begin{equation}\tag{44.12} \delta S_{\mathrm{EH}} = \frac{1}{2\kappa}\int_{\Omega}\dd^{4}x\,\sqrt{\abs{g}}\, G_{\mu\nu}\,\delta g^{\mu\nu} + \frac{1}{2\kappa}\int_{\Omega}\dd^{4}x\,\sqrt{\abs{g}}\, \nabla_{\mu}v^{\mu}\ec \end{equation}

with \(v^{\mu}\) as in Equation (44.10). For variations supported in a compact subset of the interior of \(\Omega\) the second integral vanishes, and stationarity of \(S_{\mathrm{EH}}+S_{\mathrm{m}}\) for all such variations is equivalent to the field equations Equation (44.2),

\begin{equation}\tag{44.13} G_{\mu\nu} = \kappa\,T_{\mu\nu}\ep \end{equation}

In vacuum (\(S_{\mathrm{m}}\) absent) the equations are \(G_{\mu\nu}=0\), equivalently \(R_{\mu\nu}=0\) [Hilbert:1915] [Einstein:1915b]. Rests on Lemma 44.7, Lemma 44.8 and Definition 44.6.

Proof.

Derives Theorem 44.9. Write \(\sqrt{\abs{g}}\,R =\sqrt{\abs{g}}\,g^{\mu\nu}R_{\mu\nu}\) and vary the three factors:

\begin{equation*} \delta\!\left(\sqrt{\abs{g}}\,R\right) = \delta\sqrt{\abs{g}}\;R + \sqrt{\abs{g}}\;\delta g^{\mu\nu}\,R_{\mu\nu} + \sqrt{\abs{g}}\;g^{\mu\nu}\,\delta R_{\mu\nu}\ep \end{equation*}

By Equation (44.7) the first term is \(-\tfrac12\sqrt{\abs{g}}\,g_{\mu\nu}R\,\delta g^{\mu\nu}\), which combines with the second into \(\sqrt{\abs{g}}\,G_{\mu\nu}\,\delta g^{\mu\nu}\); by Equation (44.10) the third is \(\sqrt{\abs{g}}\,\nabla_{\mu}v^{\mu}\). That is Equation (44.12).

For the divergence term, note the identity \(\Gamma^{\lambda}{}_{\lambda\mu} =\tfrac12 g^{\lambda\rho}\pp_{\mu}g_{\lambda\rho} =\pp_{\mu}\ln\sqrt{\abs{g}}\) — Jacobi's formula Equation (5.21) again — whence \(\sqrt{\abs{g}}\,\nabla_{\mu}v^{\mu} =\pp_{\mu}(\sqrt{\abs{g}}\,v^{\mu})\): a coordinate divergence. If \(\delta g_{\mu\nu}\), and with it \(v^{\mu}\), vanishes outside a compact subset of the interior, the integral of \(\pp_{\mu}(\sqrt{\abs{g}}\,v^{\mu})\) vanishes by the fundamental theorem of calculus applied coordinate by coordinate (Theorem 7.133 is its three-dimensional integral form). Adding \(\delta S_{\mathrm{m}}\) from Equation (44.5),

\begin{equation*} \delta\left(S_{\mathrm{EH}}+S_{\mathrm{m}}\right) = \int_{\Omega}\dd^{4}x\,\sqrt{\abs{g}} \left[\frac{1}{2\kappa}G_{\mu\nu} -\frac{1}{2}T_{\mu\nu}\right]\delta g^{\mu\nu}\ec \end{equation*}

and since \(\delta g^{\mu\nu}\) is an arbitrary symmetric compactly supported tensor, the fundamental lemma of the calculus of variations in its several-variable form (Lemma 16.18, as used in Theorem 16.36) gives Equation (44.13). The vacuum case and the equivalence \(G_{\mu\nu}=0\Leftrightarrow R_{\mu\nu}=0\) are Proposition 44.4.

The compact-support restriction is not a technicality to be waved away: on a region with boundary the discarded divergence is a genuine obstruction, and its repair is a boundary action in its own right.

Lemma 44.10 (Divergence theorem on $(M,g)$).

Let \(\Omega\) be a compact coordinate region whose boundary \(\pp\Omega\) is piecewise smooth and nowhere null, with outward unit conormal \(n_{\mu}\) (\(n^{\mu}n_{\mu}=\epsilon=\pm1\)), induced metric \(h_{\alpha\beta}\) and area element \(\sqrt{\abs{h}}\,\dd^{3}y\). Then for any \(C^{1}\) vector field \(v^{\mu}\),

\begin{equation}\tag{44.14} \int_{\Omega}\dd^{4}x\,\sqrt{\abs{g}}\,\nabla_{\mu}v^{\mu} = \oint_{\pp\Omega}\dd^{3}y\,\sqrt{\abs{h}}\;n_{\mu}v^{\mu}\ep \end{equation}

Rests on Theorem 7.133 and Proposition 5.2.

Proof.

Derives Lemma 44.10. As in Theorem 44.9, \(\sqrt{\abs{g}}\,\nabla_{\mu}v^{\mu} =\pp_{\mu}(\sqrt{\abs{g}}\,v^{\mu})\), and the flat divergence theorem (Theorem 7.133, in its four-dimensional form, which is proved by the identical slicing argument) turns the left side into the flux of \(\sqrt{\abs{g}}\,v^{\mu}\) through \(\pp\Omega\). It remains to identify the flux element. On a boundary face given by \(x^{1}=\text{const}\) (outward direction of increasing \(x^{1}\), the other faces being identical), the flux is \(\int\dd^{3}y\,\sqrt{\abs{g}}\,v^{1}\). By the adjugate formula for the inverse matrix (Proposition 5.49), \(g^{11}\) equals the \((1,1)\) cofactor of \(g_{\mu\nu}\) divided by \(\det g\); the cofactor is the determinant of the \(3\times3\) block of \(g\) on the coordinates \((x^{0},x^{2},x^{3})\) of the face, which is exactly \(\det h\). Hence \(\abs{g}\,\abs{g^{11}}=\abs{h}\), so \(\sqrt{\abs{g}}=\sqrt{\abs{h}}/\sqrt{\abs{g^{11}}}\) — finite precisely because the face is not null, \(g^{11}\neq0\). The outward unit conormal is \(n_{\mu}=\pp_{\mu}x^{1}/\sqrt{\abs{g^{11}}}\), with \(n^{\mu}n_{\mu}=g^{11}/\abs{g^{11}}=\epsilon\), and \(n_{\mu}v^{\mu}=v^{1}/\sqrt{\abs{g^{11}}}\). Therefore \(\sqrt{\abs{g}}\,v^{1}=\sqrt{\abs{h}}\;n_{\mu}v^{\mu}\), which is Equation (44.14).

Proposition 44.11 (The boundary term, and the Gibbons–Hawking–York action).

Let \(\pp\Omega\) be nowhere null, and consider variations with \(\delta g_{\mu\nu}=0\) on \(\pp\Omega\) but with unconstrained normal derivatives there — the boundary data of a second-order variational problem. Then the divergence term of Equation (44.12) does not vanish:

\begin{equation}\tag{44.15} n_{\mu}v^{\mu}\big|_{\pp\Omega} = -\,h^{\alpha\beta}\,n^{\rho}\,\pp_{\rho}\delta g_{\alpha\beta} = -\,2\,\delta K\ec \end{equation}

with \(K=h^{\alpha\beta}\nabla_{\alpha}n_{\beta}\) the trace of the extrinsic curvature of \(\pp\Omega\). Consequently the action with a well-defined variational principle on \(\Omega\) is not \(S_{\mathrm{EH}}\) but

\begin{equation}\tag{44.16} S_{\mathrm{EH}} + S_{\mathrm{GHY}}\ec\qquad S_{\mathrm{GHY}} = \frac{1}{\kappa}\oint_{\pp\Omega}\dd^{3}y\, \sqrt{\abs{h}}\;K\ec \end{equation}

whose total variation under these boundary conditions is \((2\kappa)^{-1}\int\sqrt{\abs{g}}\,G_{\mu\nu}\,\delta g^{\mu\nu}\) [York:1972] [Gibbons:1977]. Rests on Theorem 44.9 and Lemma 44.10.

Proof.

Derives Proposition 44.11. On \(\pp\Omega\) every term of \(v^{\mu}\) in Equation (44.11) may be written with partial derivatives, since \(\nabla\delta g=\pp\,\delta g-\Gamma\,\delta g\) and \(\delta g=0\) there. Decompose \(g^{\alpha\beta}=h^{\alpha\beta}+\epsilon^{-1}n^{\alpha}n^{\beta}\) along the boundary. In \(n_{\mu}v^{\mu}=g^{\alpha\beta}n^{\rho} (\pp_{\alpha}\delta g_{\rho\beta}-\pp_{\rho}\delta g_{\alpha\beta})\) the two \(n^{\alpha}n^{\beta}\) contributions are equal and cancel between the two terms; in the \(h^{\alpha\beta}\) part, the first term is a tangential derivative of \(\delta g\), which vanishes because \(\delta g\) vanishes identically along \(\pp\Omega\). That is the first equality of Equation (44.15).

For the second, vary \(K=h^{\alpha\beta}\nabla_{\alpha}n_{\beta}\) at fixed boundary metric. Since \(\delta g_{\mu\nu}=0\) on \(\pp\Omega\), the unit conormal \(n_{\mu}\propto\pp_{\mu}(\text{boundary function})\) and its normalization are unvaried there, and so is \(h^{\alpha\beta}\); moreover \(\delta n_{\beta}\) vanishes identically along \(\pp\Omega\), so its \(h\)-projected (tangential) derivatives vanish too, and the only surviving variation is through the connection, \(\delta(\nabla_{\alpha}n_{\beta}) =-\delta\Gamma^{\sigma}{}_{\alpha\beta}\,n_{\sigma}\). With Equation (44.8), again dropping tangential derivatives of \(\delta g\),

\begin{equation*} \delta K = -\tfrac{1}{2}\,h^{\alpha\beta}n^{\rho} \left(\pp_{\alpha}\delta g_{\rho\beta} + \pp_{\beta}\delta g_{\rho\alpha} - \pp_{\rho}\delta g_{\alpha\beta}\right) = +\tfrac{1}{2}\,h^{\alpha\beta}n^{\rho}\, \pp_{\rho}\delta g_{\alpha\beta} = -\tfrac{1}{2}\,n_{\mu}v^{\mu}\ep \end{equation*}

By Lemma 44.10 the offending term of Equation (44.12) is \((2\kappa)^{-1}\oint\sqrt{\abs{h}}\,n_{\mu}v^{\mu} =-\kappa^{-1}\oint\sqrt{\abs{h}}\,\delta K =-\,\delta S_{\mathrm{GHY}}\), using once more that \(\sqrt{\abs{h}}\) is unvaried on the boundary. Adding \(S_{\mathrm{GHY}}\) therefore cancels it identically.

Remark 44.12 (Reading the boundary term).

The obstruction arises because \(R\) contains second derivatives of the metric, so Equation (44.4) is a second-order Lagrangian whose boundary variation involves \(\pp_{n}\,\delta g\); the Gibbons–Hawking–York term subtracts exactly the offending total derivative. The same divergence appears, from the opposite direction, in the \(3+1\) split: one of the two total derivatives discarded in the ADM decomposition Equation (26.80) of Proposition 26.41 is this boundary term, as identified in Appendix A.52. Three honest caveats. The construction above assumes a nowhere-null boundary; null segments and the corners where segments meet require refinements that this treatise does not need. On non-compact regions the subtraction of a reference term is needed to make Equation (44.16) finite — that subtraction is where the ADM energy of Remark 26.45 enters. And the conventions here use the outward unit conormal throughout; the literature's explicit factors of \(\epsilon\) [Gibbons:1977] appear when the future-directed normal vector is used on spacelike segments instead, and the two bookkeepings agree.

Proposition 44.13 (First-order variation in vielbein-form variables).

Treat, in the vielbein form Equation (43.5) of the action at \(D=4\),

\begin{equation}\tag{44.17} S[e,\omega] = \frac{1}{4\kappa}\int_{M} \epsilon_{abcd}\,R^{ab}\wedge e^{c}\wedge e^{d}\ec \end{equation}

the vielbein \(e^{a}\) and the connection \(\omega^{ab}\) as independent fields (first-order or Palatini formalism), with compactly supported variations. Stationarity with respect to \(\omega\) is equivalent to the vanishing of the torsion, \(T^{a}=0\) — so that \(\omega=\omega(e)\) by Proposition 13.158 — and stationarity with respect to \(e\) then reproduces the vacuum Einstein equations \(G_{\mu\nu}=0\) of Theorem 44.9. Rests on Theorem 43.3, Proposition 13.158 and Theorem 13.156.

Proof.

Derives Proposition 44.13. The \(\omega\) equation. From the second structure equation Equation (13.312), \(\delta R^{ab}=\dd\,\delta\omega^{ab} +\delta\omega^{a}{}_{c}\wedge\omega^{cb} +\omega^{a}{}_{c}\wedge\delta\omega^{cb} =\mathrm{D}\,\delta\omega^{ab}\). The frame Levi-Civita symbol is \(\mathrm{D}\)-constant: \(\mathrm{D}\epsilon_{abcd}\) is totally antisymmetric in \(abcd\), hence proportional to \(\epsilon_{abcd}\), with coefficient the trace \(\omega^{e}{}_{e}=\eta_{ef}\,\omega^{ef}=0\) by the antisymmetry Equation (13.310). The graded Leibniz rule for \(\mathrm{D}\), applied to the one-form \(\delta\omega^{ab}\), therefore gives

\begin{equation*} \epsilon_{abcd}\,\mathrm{D}\delta\omega^{ab}\wedge e^{c}\wedge e^{d} = \dd\left(\epsilon_{abcd}\,\delta\omega^{ab}\wedge e^{c}\wedge e^{d}\right) + \epsilon_{abcd}\,\delta\omega^{ab}\wedge \mathrm{D}\!\left(e^{c}\wedge e^{d}\right)\ec \end{equation*}

where \(\dd\) replaces \(\mathrm{D}\) on the full contraction because it is a Lorentz scalar. The exact term integrates to zero, so \(\delta_{\omega}S=(4\kappa)^{-1}\!\int \epsilon_{abcd}\,\delta\omega^{ab}\wedge \mathrm{D}(e^{c}\wedge e^{d})\). With \(\mathrm{D}(e^{c}\wedge e^{d})=T^{c}\wedge e^{d}-e^{c}\wedge T^{d}\) (first structure equation, Equation (13.311)) and the relabelling symmetry of \(\epsilon_{abcd}\), the integrand equals \(2\,\epsilon_{abcd}\,\delta\omega^{ab}\wedge T^{c}\wedge e^{d}\), so the field equation is \(\epsilon_{abcd}\,T^{c}\wedge e^{d}=0\) for every pair \(ab\).

To see that this forces \(T^{a}=0\), expand \(T^{c}=\tfrac12 T^{c}{}_{ef}\,e^{e}\wedge e^{f}\) and wedge the equation with \(e^{g}\); using \(e^{e}\wedge e^{f}\wedge e^{d}\wedge e^{g} =\epsilon^{efdg}\,e^{0}\wedge e^{1}\wedge e^{2}\wedge e^{3}\) with the numerical symbol, the content is \(\epsilon_{abcd}\,\epsilon^{defg}\,T^{c}{}_{ef}=0\). The numerical contraction identity \(\epsilon^{defg}\epsilon_{dabc}=\delta^{efg}_{abc}\) (the \(3\times3\) determinant of Kronecker deltas; Lemma A.50 is its twice-contracted consequence) reduces this, after the six contractions, to

\begin{equation*} T^{g}{}_{ab} = \delta^{g}{}_{b}\,T^{c}{}_{ac} - \delta^{g}{}_{a}\,T^{c}{}_{bc}\ep \end{equation*}

Tracing \(g\) with \(b\) gives \(T^{c}{}_{ac}=4T^{c}{}_{ac}-T^{c}{}_{ac}\), so the trace vanishes, and with it the whole tensor: \(T^{a}=0\).

The \(e\) equation. On the surface \(T^{a}=0\) the connection is the unique torsion-free \(\omega(e)\) of Proposition 13.158, and substituting it back gives the second-order functional \(S[e,\omega(e)]\), which by Theorem 43.3 equals \(S_{\mathrm{EH}}[g]\) with \(g_{\mu\nu}=\eta_{ab}e^{a}{}_{\mu}e^{b}{}_{\nu}\). Now vary \(e\) in the first-order action at \(\omega=\omega(e)\): the chain rule splits the variation into the explicit \(\delta_{e}\) at fixed \(\omega\) and the induced \(\delta_{\omega}\) evaluated on \(\delta\omega(e)\) — and the latter vanishes, because \(\omega(e)\) is precisely the point where \(\delta_{\omega}S=0\). So the first-order \(e\) equation coincides with the total variation of \(S_{\mathrm{EH}}[g(e)]\), which by Theorem 44.9 and \(\delta g_{\mu\nu} =\eta_{ab}(e^{a}{}_{\mu}\,\delta e^{b}{}_{\nu} +e^{a}{}_{\nu}\,\delta e^{b}{}_{\mu})\) is \(\kappa^{-1}\!\int\sqrt{\abs{g}}\;G^{\mu\nu}\, \eta_{ab}e^{b}{}_{\nu}\,\delta e^{a}{}_{\mu}\,\dd^{4}x\). Since the vielbein is invertible, stationarity for all \(\delta e^{a}{}_{\mu}\) is equivalent to \(G^{\mu\nu}=0\).

Remark 44.14 (The priority question).

Hilbert's Göttingen communication is dated 20 November 1915, five days before Einstein's [Hilbert:1915] [Einstein:1915b], and for eighty years the field equations were sometimes said to have been found first by Hilbert. The printer's proofs of Hilbert's paper, recovered in 1997, show that the explicit field equations were not present in the version submitted on 20 November and entered only in revision, after Einstein's paper had appeared; the published version also carries a December revision date [Corry:1997]. What is securely Hilbert's is the action route itself — the recognition that Equation (44.4) is the scalar whose variation does the work, which this section has followed.

The stress–energy tensor

Matter models

Definition 44.6 assigns every covariantly coupled matter action a symmetric stress–energy tensor. Three models carry all the matter physics this part needs [Misner:1973] [Landau:1975]; their special-relativistic particle content — four-momentum and its conservation — is Relativistic Dynamics.

Definition 44.15 (Dust).

A pressureless fluid — dust — with proper mass density \(\rho\) (in \(\mathrm{kg}/\mathrm{m}^{3}\)) and four-velocity field \(u^{\mu}\) (\(u^{\mu}u_{\mu}=-c^{2}\), Definition 40.2) has

\begin{equation}\tag{44.18} T^{\mu\nu} = \rho\,u^{\mu}u^{\nu}\ep \end{equation}

In the local rest frame \(T^{00}=\rho c^{2}\) — the rest energy density of Phenomenon 40.6 — and all other components vanish. Rests on Definition 40.2 and Phenomenon 40.6.

Definition 44.16 (Perfect fluid).

A fluid with proper energy density \(\rho c^{2}\) (internal energy included), proper pressure \(p\) (in \(\mathrm{Pa}\)), and four-velocity \(u^{\mu}\), but no viscosity and no heat flux, has

\begin{equation}\tag{44.19} T^{\mu\nu} = \left(\rho+\frac{p}{c^{2}}\right)u^{\mu}u^{\nu} + p\,g^{\mu\nu}\ep \end{equation}

In the local rest frame \(T^{\mu\nu}=\diag(\rho c^{2},p,p,p)\): isotropic pressure, no energy flux. Dust is the case \(p=0\); radiation the case \(p=\rho c^{2}/3\), for which the trace \(T=-\rho c^{2}+3p\) vanishes. Rests on Definition 44.15.

Proposition 44.17 (Stress–energy of the electromagnetic field).

The Maxwell action in curved spacetime,

\begin{equation}\tag{44.20} S_{\mathrm{EM}} = -\frac{1}{4\mu_{0}}\int\dd^{4}x\,\sqrt{\abs{g}}\; F_{\alpha\beta}F^{\alpha\beta}\ec \end{equation}

with \(F_{\mu\nu}=\pp_{\mu}A_{\nu}-\pp_{\nu}A_{\mu}\) the field tensor of The Maxwell Equations, yields

\begin{equation}\tag{44.21} T_{\mu\nu} = \frac{1}{\mu_{0}}\left( F_{\mu}{}^{\alpha}F_{\nu\alpha} - \tfrac{1}{4}\,g_{\mu\nu}\,F_{\alpha\beta}F^{\alpha\beta} \right)\ep \end{equation}

It is traceless, \(g^{\mu\nu}T_{\mu\nu}=0\), and its time–time component in any local orthonormal frame is the familiar energy density \(\epsilon_{0}E^{2}/2+B^{2}/2\mu_{0}\). Rests on Definition 44.6 and Lemma 44.7.

Proof.

Derives Proposition 44.17. \(F_{\mu\nu}\), defined from the potential with lower indices, does not involve the metric; all metric dependence of Equation (44.20) sits in the two raised indices and the volume factor. Varying,

\begin{equation*} \delta S_{\mathrm{EM}} = -\frac{1}{4\mu_{0}}\int\dd^{4}x\left[ \delta\sqrt{\abs{g}}\;F_{\alpha\beta}F^{\alpha\beta} + \sqrt{\abs{g}}\;2F_{\mu\alpha}F_{\nu\beta}\,g^{\alpha\beta}\, \delta g^{\mu\nu}\right]\ec \end{equation*}

and inserting Equation (44.7) for the first term,

\begin{equation*} \delta S_{\mathrm{EM}} = -\frac{1}{2}\int\dd^{4}x\,\sqrt{\abs{g}}\; \frac{1}{\mu_{0}}\left(F_{\mu}{}^{\alpha}F_{\nu\alpha} -\tfrac14 g_{\mu\nu}F_{\alpha\beta}F^{\alpha\beta}\right) \delta g^{\mu\nu}\ec \end{equation*}

which by Equation (44.5) is Equation (44.21). The trace is \(\mu_{0}^{-1}(F^{\nu\alpha}F_{\nu\alpha} -\tfrac14\cdot4\,F_{\alpha\beta}F^{\alpha\beta})=0\), a special feature of \(D=4\). For the energy density, work in a local orthonormal frame: \(F_{0}{}^{\alpha}F_{0\alpha}=g^{ij}F_{0i}F_{0j}=E^{2}/c^{2}\) and \(F_{\alpha\beta}F^{\alpha\beta}=2(B^{2}-E^{2}/c^{2})\), so

\begin{equation*} T_{00} = \frac{1}{\mu_{0}}\left[\frac{E^{2}}{c^{2}} + \frac{1}{2}\left(B^{2}-\frac{E^{2}}{c^{2}}\right)\right] = \frac{\epsilon_{0}E^{2}}{2}+\frac{B^{2}}{2\mu_{0}}\ec \end{equation*}

using \(\epsilon_{0}\mu_{0}=1/c^{2}\); both intermediate quantities are squares, so the identification is independent of the sign convention relating \(F_{0i}\) to \(E_{i}\).

Remark 44.18 (Hilbert versus canonical tensor).

Translation invariance already gives every flat-spacetime field theory a conserved energy–momentum tensor by Noether's first theorem — the canonical tensor Equation (16.83) of Corollary 16.91 — but that tensor is in general not symmetric, and only becomes so after adding an identically conserved improvement term. The metric definition Equation (44.5) is symmetric from the start, and for the Maxwell field it reproduces exactly the improved (symmetrized) canonical tensor; the systematic statement of that equivalence, the Belinfante construction, belongs to Generalized Classical Field Theory (Sections 64.4.2 and 64.4.3). It is the metric tensor, not the canonical one, that gravity couples to: the right-hand side of Equation (44.2) is defined by the same variation that produces the left-hand side.

Conservation and Noether's theorem

Theorem 44.19 (Covariant conservation of stress–energy).

Let \(S_{\mathrm{m}}[\psi;g]\) be diffeomorphism invariant, and let the matter fields satisfy their own Euler–Lagrange equations. Then

\begin{equation}\tag{44.22} \nabla_{\mu}T^{\mu\nu} = 0\ep \end{equation}

Rests on Theorem 16.93, Definition 44.6 and Proposition 13.127.

Proof.

Derives Theorem 44.19. Let \(\xi^{\mu}\) be an arbitrary compactly supported vector field and drag all fields along its flow. Diffeomorphism invariance says the action does not change: \(0=\delta_{\xi}S_{\mathrm{m}} =\int(\delta S_{\mathrm{m}}/\delta\psi)\,\delta_{\xi}\psi +\int(\delta S_{\mathrm{m}}/\delta g^{\mu\nu})\, \delta_{\xi}g^{\mu\nu}\). On shell the first integral vanishes. For the second, the Lie derivative of the metric is \(\delta_{\xi}g_{\mu\nu} =\nabla_{\mu}\xi_{\nu}+\nabla_{\nu}\xi_{\mu}\) (Equation (13.275) with \(\pp\to\nabla\) by metricity, as in the proof of Killing's equation Equation (13.290)), so by Equations (44.5) and (44.6)

\begin{equation*} 0 = +\frac{1}{2}\int\dd^{4}x\,\sqrt{\abs{g}}\; T^{\mu\nu}\left(\nabla_{\mu}\xi_{\nu} +\nabla_{\nu}\xi_{\mu}\right) = \int\dd^{4}x\,\sqrt{\abs{g}}\; T^{\mu\nu}\nabla_{\mu}\xi_{\nu}\ec \end{equation*}

using the symmetry of \(T^{\mu\nu}\). Integrate by parts with Lemma 44.10 (no boundary term, compact support): \(0=-\int\sqrt{\abs{g}}\,(\nabla_{\mu}T^{\mu\nu})\,\xi_{\nu}\), and since \(\xi_{\nu}\) is arbitrary, Equation (44.22) follows. This is Noether's second theorem (Theorem 16.93) in action: the symmetry group depends on four arbitrary functions \(\xi^{\mu}\), and what it yields is not four conserved charges but four differential identities [Noether:1918].

Proposition 44.20 (Perfect-fluid equations of motion).

For the perfect fluid Equation (44.19), Equation (44.22) splits along \(u^{\mu}\) and orthogonally to it into

\begin{align} \nabla_{\mu}\left(\rho u^{\mu}\right) &= -\frac{p}{c^{2}}\,\nabla_{\mu}u^{\mu}\ec \tag{44.23}\\ \left(\rho+\frac{p}{c^{2}}\right)u^{\mu}\nabla_{\mu}u^{\lambda} &= -\left(g^{\lambda\nu} +\frac{u^{\lambda}u^{\nu}}{c^{2}}\right)\pp_{\nu}p\ec \tag{44.24} \end{align}

the relativistic continuity and Euler equations. In the limit \(\abs{\vect{v}}\ll c\), \(p\ll\rho c^{2}\) they reduce to the continuity and Euler equations of Fluid Dynamics. Rests on Theorem 44.19 and Definition 44.16.

Proof.

Derives Proposition 44.20. Insert Equation (44.19) into \(\nabla_{\mu}T^{\mu\lambda}=0\):

\begin{equation*} \nabla_{\mu}\!\left[\left(\rho+\tfrac{p}{c^{2}}\right) u^{\mu}\right]u^{\lambda} + \left(\rho+\tfrac{p}{c^{2}}\right)u^{\mu} \nabla_{\mu}u^{\lambda} + g^{\lambda\nu}\pp_{\nu}p = 0\ep \end{equation*}

Contract with \(u_{\lambda}\): since \(u_{\lambda}u^{\lambda}=-c^{2}\) is constant, \(u_{\lambda}\nabla_{\mu}u^{\lambda}=0\), so the middle term dies, the first gives \(-c^{2}\nabla_{\mu}[(\rho+p/c^{2})u^{\mu}]\), and the last gives \(u^{\mu}\pp_{\mu}p\). Expanding \(\nabla_{\mu}[(p/c^{2})u^{\mu}] =(p/c^{2})\nabla_{\mu}u^{\mu}+(u^{\mu}/c^{2})\pp_{\mu}p\), the two pressure-gradient terms cancel and what remains, divided by \(-c^{2}\), is exactly Equation (44.23). Projecting instead with \(h^{\lambda}{}_{\sigma} =\delta^{\lambda}{}_{\sigma}+u^{\lambda}u_{\sigma}/c^{2}\), which annihilates \(u^{\lambda}\), kills the first term and produces Equation (44.24). In the nonrelativistic limit \(u^{\mu}\to(c,\vect{v})\), \(\nabla\to\pp\), \(\rho+p/c^{2}\to\rho\) and the projector becomes spatial; Equation (44.23) becomes \(\pp_{t}\rho+\nabla\cdot(\rho\vect{v})=0\) and Equation (44.24) becomes \(\rho(\pp_{t}+\vect{v}\cdot\nabla)\vect{v}=-\nabla p\), the equations of Fluid Dynamics.

Corollary 44.21 (Dust flows on geodesics).

For dust (\(p=0\)), Equation (44.24) reduces to \(u^{\mu}\nabla_{\mu}u^{\lambda}=0\): the integral curves of \(u^{\mu}\) are timelike geodesics. The geodesic postulate Postulate 43.1 is therefore not independent of the field equations for this matter model: conservation of the source, itself enforced by the field equations (Corollary 44.24), already moves the matter on geodesics. Rests on Proposition 44.20 and Postulate 43.1.

Proof.

Derives Corollary 44.21. Set \(p=0\) in Equation (44.24); the right side vanishes and the left is \(\rho\) times the geodesic equation Equation (43.1) in its velocity-field form.

Remark 44.22 (What covariant conservation does and does not conserve).

In flat spacetime \(\pp_{\mu}T^{\mu\nu}=0\) integrates to four conserved charges. The covariant law Equation (44.22) does not: the connection terms act as sources, describing the exchange of energy and momentum between matter and the gravitational field, and no coordinate-independent gravitational energy density exists to book the exchange against — by the equivalence principle, the connection can be made to vanish at any one event, taking any candidate density with it. What survives is either of two honest substitutes. With a symmetry: a Killing vector \(\xi\) makes \(T^{\mu\nu}\xi_{\nu}\) a genuinely conserved current, by Equation (44.22) and Killing's equation Equation (13.290). With asymptotic flatness: the total energy, momentum and angular momentum of an isolated system are boundary integrals at spatial infinity — the ADM integrals, whose constrained-dynamics origin is Remark 26.45 [Arnowitt:1962]. Between the two sits the Landau–Lifshitz pseudotensor [Landau:1975], coordinate-dependent by construction, useful because its integrals reproduce the ADM quantities in asymptotically Cartesian coordinates; the energy carried by gravitational waves, computed via the closely related Isaacson average in Appendix A.1, is the one place this part meets the issue quantitatively.

The Bianchi identities

The differential identities of the curvature tensor are established, in both index and Cartan form, in Differentiable Manifolds, Tensors, and Curvature: the first and second Bianchi identities are Equation (13.308) and, as two lines of form algebra, Proposition 13.157. The customary attribution to Bianchi [Bianchi:1902] is loose — the identities were known to Voss in 1880 and within Ricci's school — and this treatise keeps the customary name while recording the fact. What Part II deliberately does not do is contract them (Remark 16.95 notes the omission); the contraction is where the physics lives, and it is performed here.

Theorem 44.23 (Contracted Bianchi identity).

For the Levi-Civita connection,

\begin{equation}\tag{44.25} \nabla^{\mu}G_{\mu\nu} = 0\ec \qquad\text{equivalently}\qquad \nabla^{\mu}R_{\mu\nu}=\tfrac{1}{2}\,\pp_{\nu}R\ep \end{equation}

Rests on Proposition 13.154, Definition 13.149 and Definition 44.2.

Proof.

Derives Theorem 44.23. Write the second Bianchi identity of Equation (13.308) with its cycle explicit,

\begin{equation*} \nabla_{\sigma}R^{\lambda}{}_{\rho\mu\nu} + \nabla_{\mu}R^{\lambda}{}_{\rho\nu\sigma} + \nabla_{\nu}R^{\lambda}{}_{\rho\sigma\mu} = 0\ep \end{equation*}

Contract \(\lambda\) with \(\mu\) (legitimate under \(\nabla\) by metricity): the first term gives \(\nabla_{\sigma}R_{\rho\nu}\); the third, by antisymmetry in the last index pair, \(-\nabla_{\nu}R_{\rho\sigma}\); the second stays \(\nabla_{\lambda}R^{\lambda}{}_{\rho\nu\sigma}\):

\begin{equation}\tag{44.26} \nabla_{\sigma}R_{\rho\nu} - \nabla_{\nu}R_{\rho\sigma} + \nabla_{\lambda}R^{\lambda}{}_{\rho\nu\sigma} = 0\ep \end{equation}

Now contract with \(g^{\rho\sigma}\). The first term gives \(\nabla^{\rho}R_{\rho\nu}\) and the second \(-\pp_{\nu}R\). In the third, lower the index, \(g^{\rho\sigma}R^{\lambda}{}_{\rho\nu\sigma} =g^{\rho\sigma}g^{\lambda\alpha}R_{\alpha\rho\nu\sigma}\), and use the pair-exchange symmetry of Equation (13.308) followed by antisymmetry in each pair:

\begin{equation*} g^{\rho\sigma}R_{\alpha\rho\nu\sigma} = g^{\rho\sigma}R_{\nu\sigma\alpha\rho} = g^{\rho\sigma}\left(-1\right)\left(-1\right) R_{\sigma\nu\rho\alpha} = R^{\rho}{}_{\nu\rho\alpha} = R_{\nu\alpha}\ec \end{equation*}

the last step being the Ricci contraction Equation (13.307) of the first and third slots. So the third term is \(\nabla_{\lambda}(g^{\lambda\alpha}R_{\nu\alpha}) =\nabla^{\rho}R_{\rho\nu}\). Altogether \(2\nabla^{\rho}R_{\rho\nu}=\pp_{\nu}R\), and

\begin{equation*} \nabla^{\mu}G_{\mu\nu} = \nabla^{\mu}R_{\mu\nu} - \tfrac12\,g_{\mu\nu}\nabla^{\mu}R = \tfrac12\,\pp_{\nu}R - \tfrac12\,\pp_{\nu}R = 0\ep \end{equation*}
Corollary 44.24 (Conservation is an integrability condition).

Any metric satisfying Equation (44.2) has \(\nabla_{\mu}T^{\mu\nu}=0\) automatically. Local energy–momentum conservation is therefore not an extra postulate of general relativity: it is the integrability condition of the field equations, exactly as charge conservation is the integrability condition of the Maxwell equations (Remark 16.95). Conversely, a candidate left-hand side that is not identically divergence-free could not consistently couple to conserved matter — the flaw that doomed Einstein's 1913–1915 intermediate theories (Section 44.1.2). Rests on Theorem 44.23 and Postulate 44.3.

Proof.

Derives Corollary 44.24. Apply \(\nabla^{\mu}\) to both sides of Equation (44.2) and use Equation (44.25).

Remark 44.25 (Ten equations, four identities).

Equation (44.25) is four differential identities among the ten field equations, so at most six are independent — the situation anticipated in general form by Corollary 16.94: the identities are the Noether identities of the four-parameter diffeomorphism freedom. The count is exactly right, not a defect: four of the ten \(g_{\mu\nu}\) are gauge (coordinate choice), and the four equations “lost” to the identities resurface as constraints on initial data rather than evolution equations. That story is Section 44.9.

The Newtonian correspondence

Geodesics and the potential

Proposition 44.26 (Newtonian limit of geodesic motion).

Let the metric be static and weakly curved,

\begin{equation}\tag{44.27} g_{00} = -\left(1+\frac{2\Phi}{c^{2}}\right)\ec\qquad g_{0i} = 0\ec\qquad g_{ij} = \delta_{ij} + O\!\left(\Phi/c^{2}\right)\ec \end{equation}

with \(\abs{\Phi}\ll c^{2}\) time-independent, and let a test body move slowly, \(\abs{\dd x^{i}/\dd t}\ll c\). Then the geodesic equation Equation (43.1) reduces to Newton's second law in the potential \(\Phi\),

\begin{equation}\tag{44.28} \frac{\dd^{2}x^{i}}{\dd t^{2}} = -\,\pp_{i}\Phi\ec \end{equation}

identifying \(\Phi\) (in \(\mathrm{m}^{2}/\mathrm{s}^{2}\)) with the Newtonian gravitational potential of Newtonian Dynamics and Central Forces and Statics. Rests on Postulate 43.1.

Proof.

Derives Proposition 44.26. For slow motion \(\dd x^{i}/\dd\tau\ll\dd x^{0}/\dd\tau\) and \(\dd x^{0}/\dd\tau=c\,\dd t/\dd\tau\approx c\), so among the \(\Gamma^{i}{}_{\mu\nu}\,\dot{x}^{\mu}\dot{x}^{\nu}\) terms of Equation (43.1) only \(\Gamma^{i}{}_{00}(\dot{x}^{0})^{2}\) survives at leading order. For a static metric,

\begin{equation*} \Gamma^{i}{}_{00} = \tfrac12 g^{i\rho} \left(2\pp_{0}g_{\rho0}-\pp_{\rho}g_{00}\right) = -\tfrac12\,g^{ij}\pp_{j}g_{00} = -\tfrac12\,\delta^{ij}\pp_{j} \left(-\frac{2\Phi}{c^{2}}\right) + O(\Phi^{2}/c^{4}) = \frac{\pp_{i}\Phi}{c^{2}}\ec \end{equation*}

where the spatial perturbation in \(g^{ij}\) multiplies a quantity already \(O(\Phi)\) and drops. Hence \(\dd^{2}x^{i}/\dd\tau^{2}=-c^{2}\,\Gamma^{i}{}_{00}=-\pp_{i}\Phi\) and, since \(\dd\tau\approx\dd t\) at this order, Equation (44.28). Note that only \(g_{00}\) enters: the identification of the potential is insensitive to the spatial part of Equation (44.27). The same \(g_{00}\) is what the gravitational-redshift measurements read directly (Phenomenon 42.5).

Fixing the coupling constant

Theorem 44.27 (Newtonian correspondence of the field equations).

For the static weak field Equation (44.27) sourced by static dust of density \(\rho\), the time–time component of the field equations Equation (44.2) reduces to the Poisson equation

\begin{equation}\tag{44.29} \nabla^{2}\Phi = \frac{\kappa c^{4}}{2}\,\rho\ec \end{equation}

and correspondence with Newtonian gravity, \(\nabla^{2}\Phi=4\pi G\rho\), fixes

\begin{equation}\tag{44.30} \kappa = \frac{8\pi G}{c^{4}} \approx 2.0766\times 10^{-43}\,\mathrm{s}^{2}/\mathrm{kg}/\mathrm{m}\ec \end{equation}

with \(G\) the constant measured in Experiment: The Cavendish Torsion Balance [Einstein:1915b]. Rests on Proposition 44.4, Proposition 44.26 and Definition 44.15.

Proof.

Derives Theorem 44.27. Work in the trace-reversed form Equation (44.3). For static dust at rest, Equation (44.18) gives \(T_{00}=\rho c^{2}\), the other components vanishing, and \(T=g^{\mu\nu}T_{\mu\nu}=-\rho c^{2}\) to leading order. Hence

\begin{equation*} R_{00} = \kappa\left(T_{00}-\tfrac12 g_{00}T\right) = \kappa\left(\rho c^{2} -\tfrac12(-1)(-\rho c^{2})\right) = \tfrac12\,\kappa\rho c^{2}\ep \end{equation*}

On the geometric side, the Ricci contraction of Equation (13.306) is \(R_{00}=\pp_{\lambda}\Gamma^{\lambda}{}_{00} -\pp_{0}\Gamma^{\lambda}{}_{\lambda0}+O(\Gamma^{2})\); the \(\Gamma^{2}\) terms are \(O(\Phi^{2}/c^{4})\) and every time derivative vanishes, so with \(\Gamma^{i}{}_{00}=\pp_{i}\Phi/c^{2}\) from Proposition 44.26,

\begin{equation*} R_{00} = \pp_{i}\Gamma^{i}{}_{00} = \frac{\nabla^{2}\Phi}{c^{2}}\ep \end{equation*}

Equating the two expressions gives Equation (44.29). The Newtonian side is the field form of the inverse-square law: for a point mass, \(\Phi=-Gm/\abs{\vect{x}}\) (Central Forces and Statics), and superposing over a continuous density, \(\Phi(\vect{x})=-G\int\rho(\vect{x}')\, \abs{\vect{x}-\vect{x}'}^{-1}\dd^{3}x'\), the fundamental-solution property of \(-1/4\pi\abs{\vect{x}}\) (Proposition 10.67) gives \(\nabla^{2}\Phi=4\pi G\rho\). Matching coefficients, \(\kappa c^{4}/2=4\pi G\), which is Equation (44.30); the numerical value uses the CODATA \(G\) of Appendix B, whose laboratory determination is Experiment: The Cavendish Torsion Balance.

Remark 44.28 (What the Newtonian limit does and does not fix).

The correspondence reads only \(g_{00}\) and only the trace-reversed time–time equation; it fixes the single constant \(\kappa\) and nothing else. It does not test the spatial part of the weak-field metric — that is done by light deflection and the Shapiro delay, which measure exactly the spatial curvature the Newtonian limit is blind to, and which decided against Einstein's own 1911 half-value (Section 42.5, Experiment: The Classical Tests of General Relativity); in the parametrized post-Newtonian language the limit fixes no PPN parameter at all, while the classical tests fix \(\gamma\) and \(\beta\) [Will:2014]. Nor does the limit exclude a cosmological term: \(\Lambda\) adds to Equation (44.29) a contribution \(-\Lambda c^{2}\) — a constant outward acceleration \(\Lambda c^{2}r/3\) — utterly negligible at solar-system scales for the measured value of Remark 44.32, which is why Section 44.6 must be settled by cosmology rather than by laboratory gravity.

The linearized theory

Far from strong sources spacetime is nearly flat, and the field equations linearize. The full derivation — linearized curvature, gauge fixing, wave solutions, energy flux and the quadrupole formula — is carried out once, in Appendix A.1; this section states the equations, since both Gravitational-Wave Theory and the cosmological perturbation theory of Evidence-Based Cosmology start from them.

Proposition 44.29 (Linearized field equations).

Write \(g_{\mu\nu}=\eta_{\mu\nu}+h_{\mu\nu}\) with \(\abs{h_{\mu\nu}}\ll1\), raise and lower indices with \(\eta\), and set \(h=\eta^{\mu\nu}h_{\mu\nu}\). To first order in \(h\):

  1. The Einstein tensor is

    \begin{equation}\tag{44.31} G_{\mu\nu} = \tfrac{1}{2}\left( \pp_{\rho}\pp_{\mu}h^{\rho}{}_{\nu} + \pp_{\rho}\pp_{\nu}h^{\rho}{}_{\mu} - \Box h_{\mu\nu} - \pp_{\mu}\pp_{\nu}h - \eta_{\mu\nu}\pp_{\rho}\pp_{\sigma}h^{\rho\sigma} + \eta_{\mu\nu}\Box h\right)\ec \end{equation}

    with \(\Box=\eta^{\alpha\beta}\pp_{\alpha}\pp_{\beta}\).

  2. Under an infinitesimal coordinate change \(x^{\mu}\to x^{\mu}+\xi^{\mu}\) (with \(\pp\xi\) of order \(h\)),

    \begin{equation}\tag{44.32} h_{\mu\nu}\;\longrightarrow\; h_{\mu\nu}-\pp_{\mu}\xi_{\nu}-\pp_{\nu}\xi_{\mu}\ec \end{equation}

    and Equation (44.31) is invariant, as is the linearized Riemann tensor.

  3. The Lorenz gauge \(\pp^{\mu}\bar h_{\mu\nu}=0\), with \(\bar h_{\mu\nu}=h_{\mu\nu}-\tfrac12\eta_{\mu\nu}h\) the trace-reversed perturbation, is always attainable, and in it the field equations Equation (44.2) collapse to the inhomogeneous wave equation

    \begin{equation}\tag{44.33} \Box\,\bar h_{\mu\nu} = -\,2\kappa\,T_{\mu\nu} = -\,\frac{16\pi G}{c^{4}}\,T_{\mu\nu}\ec \end{equation}

    which is Equation (46.2) [Einstein:1916] [Misner:1973] [Wald:1984].

Rests on Postulate 44.3 and Theorem 44.27.

Derives Proposition 44.29.

The proof is the opening of Appendix A.1: Equation (44.31) is Equation (A.9), assembled from the linearized Christoffel symbols and Riemann tensor Equations (A.4) and (A.6); the gauge transformation Equation (44.32) is Equation (A.16); the attainability of the Lorenz gauge and the reduction to Equation (44.33) are Equations (A.20) and (A.21).

Three comments place the result. First, Equation (44.33) is the whole causal structure of the theory in miniature: disturbances of the metric propagate at speed \(c\), sourced by stress–energy — the qualitative break with the instantaneous Poisson equation that requirement (iii) of Section 44.1.1 preserved only as a limit. Second, the residual gauge freedom inside the Lorenz class reduces the ten \(h_{\mu\nu}\) to two physical polarizations; the transverse-traceless construction is Section 46.2, and the same count falls out of the exact Hamiltonian analysis, with no linearization, in Theorem 26.42. Third, the history: Einstein integrated Equation (44.33) approximately in 1916 [Einstein:1916] and corrected the radiation formula in 1918 [Einstein:1918]; the theory of the waves is Gravitational-Wave Theory and their observation — indirect through the binary pulsar, direct with the LIGO interferometers — is Experiment: Gravitational Waves.

The cosmological constant

Proposition 44.30 (The cosmological term).

For any constant \(\Lambda\) (SI dimension \(/\mathrm{m}^{2}\)), the equations

\begin{equation}\tag{44.34} G_{\mu\nu} + \Lambda\,g_{\mu\nu} = \kappa\,T_{\mu\nu} \end{equation}

retain every structural property of Equation (44.2): the left side is symmetric, built from \(g\) and its first two derivatives, and identically divergence-free, since \(\nabla_{\lambda}g_{\mu\nu}=0\) by metricity. They follow from the action Equation (44.4) with \(R\) replaced by \(R-2\Lambda\). By Theorem 44.33 below, this one-parameter enlargement is the only one available in four dimensions. Rests on Theorem 44.9, Definition 13.149 and Theorem 44.23.

Proof.

Derives Proposition 44.30. Divergence-freedom is \(\nabla^{\mu}(\Lambda g_{\mu\nu})=\Lambda\nabla^{\mu}g_{\mu\nu}=0\) together with Equation (44.25). For the action route, the extra term is \(-(\Lambda/\kappa)\int\dd^{4}x\sqrt{\abs{g}}\), whose variation by Equation (44.7) is \(+(\Lambda/2\kappa)\int\sqrt{\abs{g}}\,g_{\mu\nu}\delta g^{\mu\nu}\); added to Equation (44.12) it shifts \(G_{\mu\nu}\to G_{\mu\nu}+\Lambda g_{\mu\nu}\) in Equation (44.13).

Einstein introduced the term in 1917, to permit a static, spatially closed universe of uniform dust — the balance requires \(\Lambda=4\pi G\rho/c^{2}\), with the curvature radius \(1/\sqrt{\Lambda}\) [Einstein:1917a]. The motive did not survive: the balance is unstable, a slight expansion diluting the dust and unbalancing the repulsion further, as Eddington showed in 1930 [Eddington:1930], and the observed expansion of the universe removed the desire for a static solution altogether; the dynamical (Friedmann) analysis in which both statements live belongs to Section 48.2.2. What survived is the term itself.

Proposition 44.31 (de Sitter geometry).

With \(T_{\mu\nu}=0\) and \(\Lambda>0\), the maximally symmetric solution of Equation (44.34) has

\begin{equation}\tag{44.35} R_{\mu\nu}=\Lambda\,g_{\mu\nu}\ec\qquad R = 4\Lambda\ec\qquad R_{\lambda\rho\mu\nu} = \frac{\Lambda}{3}\left(g_{\lambda\mu}g_{\rho\nu} - g_{\lambda\nu}g_{\rho\mu}\right)\ec \end{equation}

the constant-curvature spacetime of curvature radius \(\ell=\sqrt{3/\Lambda}\): de Sitter space, realized as a quadric in five flat dimensions in Section 13.13 [deSitter:1917]. \(\Lambda\) alone, with no matter whatever, curves spacetime. Rests on Theorem 13.160 and Proposition 44.30.

Proof.

Derives Proposition 44.31. By Theorem 13.160 a maximally symmetric metric has \(R_{\lambda\rho\mu\nu} =\tfrac{R}{12}(g_{\lambda\mu}g_{\rho\nu} -g_{\lambda\nu}g_{\rho\mu})\) with \(R\) constant, whence \(R_{\mu\nu}=\tfrac{R}{4}g_{\mu\nu}\). Insert into Equation (44.34) with \(T=0\): \(\tfrac{R}{4}g_{\mu\nu}-\tfrac{R}{2}g_{\mu\nu} +\Lambda g_{\mu\nu}=0\), so \(R=4\Lambda\), and back-substitution gives Equation (44.35). The curvature constant of Equation (13.318) is \(R/12=\Lambda/3\), giving \(\ell=(3/\Lambda)^{1/2}\); existence is the explicit quadric construction of Section 13.13. The case \(\Lambda<0\) gives anti-de Sitter space the same way.

Remark 44.32 (The measured cosmological constant).

\(\Lambda\) is today a measured cosmological parameter, not an option. The accelerating expansion discovered in the type-Ia supernova surveys [Riess:1998] [Perlmutter:1999] (Phenomenon 48.17) and the CMB-anchored fits of [Aghanim:2020] concordantly give, through \(\Lambda=3\Omega_{\Lambda}H_{0}^{2}/c^{2}\) with \(\Omega_{\Lambda}\approx0.685\) and \(H_{0}\approx67.4\,\mathrm{km}/\mathrm{s}/\mathrm{Mpc}\),

\begin{equation}\tag{44.36} \Lambda \approx 1.1\times 10^{-52}\,/\mathrm{m}^{2}\ec \end{equation}

equivalently a vacuum energy density \(\rho_{\Lambda}c^{2}=\Lambda c^{4}/8\pi G \approx5.3\times 10^{-10}\,\mathrm{J}/\mathrm{m}^{3}\) — about half a nanojoule per cubic metre. Moved to the right-hand side of Equation (44.34), the term is a perfect fluid with \(p=-\rho c^{2}\), which is what makes it gravitationally repulsive (Remark 44.40). Why it is so small is not known: naive quantum-field-theoretic estimates of vacuum energy exceed the measured value by up to some 120 orders of magnitude, depending on the cutoff assumed — the cosmological-constant problem, stated sharply in [Weinberg:1989]. The observational treatment of \(\Lambda\), and of the broader dark-energy question, is Evidence-Based Cosmology (Section 48.6.2).

Lovelock's uniqueness theorem

The requirements of Section 44.1.1 were presented as motivation; remarkably, they are a characterization. The following theorem is imported: its proof is a classification of tensor concomitants that belongs to the mathematical literature, and this treatise uses only its statement.

Theorem 44.33 (Lovelock's uniqueness theorem; imported).

In four dimensions, let \(A^{\mu\nu}\) be a tensor concomitant of the metric and its first and second partial derivatives, \(A^{\mu\nu}=A^{\mu\nu}(g_{\alpha\beta}, \pp_{\gamma}g_{\alpha\beta},\pp_{\gamma}\pp_{\delta}g_{\alpha\beta})\), satisfying \(\nabla_{\mu}A^{\mu\nu}=0\) identically. Then there exist constants \(\alpha\) and \(\lambda\) with

\begin{equation}\tag{44.37} A^{\mu\nu} = \alpha\,G^{\mu\nu} + \lambda\,g^{\mu\nu}\ep \end{equation}

Neither symmetry of \(A^{\mu\nu}\) nor linearity in the second derivatives needs to be assumed: in \(D=4\) both follow [Lovelock:1971] [Lovelock:1972]. Rests on Definition 44.2 and Theorem 44.23.

Remark 44.34 (Status and scope of the import).

The proof is in Lovelock's two papers: the 1971 paper [Lovelock:1971] classifies the divergence-free symmetric concomitants in arbitrary dimension, and the 1972 paper [Lovelock:1972] shows that in four dimensions the symmetry and linearity hypotheses are redundant. The statement is naturally dimension-general in the sense of the Part II conventions: in \(D>4\) the classification admits further terms, one for each even dimension below \(D\) — the Lovelock tensors, obtained by varying dimensionally continued Euler densities, of which the first beyond Einstein is the quadratic Gauss–Bonnet combination \(R^{2}-4R_{\mu\nu}R^{\mu\nu} +R_{\lambda\rho\mu\nu}R^{\lambda\rho\mu\nu}\). In \(D=4\) that combination is the Euler density itself: a topological term whose variation vanishes identically, contributing nothing to the field equations — which is precisely why the four-dimensional answer Equation (44.37) is so short. Physical spacetime instantiates \(D=4\), and only Equation (44.37) is used in this treatise.

Corollary 44.35 (The field equations are essentially unique).

Any four-dimensional theory meeting the requirements of Section 44.1.1 — metric field variable, tensorial second-order field equations, identically conserved left-hand side coupled to the stress–energy tensor — has field equations of the form \(\alpha G_{\mu\nu}+\lambda g_{\mu\nu}=T_{\mu\nu}\); absorbing the normalization into \(\kappa=1/\alpha\) and writing \(\Lambda=\lambda/\alpha\), these are Equation (44.34). The Newtonian limit then fixes \(\kappa\) (Theorem 44.27), and observation fixes \(\Lambda\) (Remark 44.32). Nothing else was available. Rests on Theorems 44.27 and 44.33.

Proof.

Derives Corollary 44.35. Immediate from Theorem 44.33 applied to the left-hand side, plus the two calibrations cited.

Energy conditions

The field equations place no restriction whatever on \(T_{\mu\nu}\): any metric solves them for some source. Physical conclusions therefore need model-independent positivity assumptions about matter, and four standard ones do nearly all the work in this part — above all as hypotheses of the singularity theorems of Section 45.4.2 [Hawking:1973] [Penrose:1965].

Definition 44.36 (Energy conditions).

Let \(w^{\mu}\) range over future-directed timelike vectors with \(w^{\mu}w_{\mu}=-c^{2}\), and \(k^{\mu}\) over future-directed null vectors. The stress–energy tensor satisfies the

  • null energy condition (NEC) if \(T_{\mu\nu}k^{\mu}k^{\nu}\ge0\) for all \(k\);

  • weak energy condition (WEC) if \(T_{\mu\nu}w^{\mu}w^{\nu}\ge0\) for all \(w\) — every observer measures nonnegative energy density;

  • strong energy condition (SEC) if \((T_{\mu\nu}-\tfrac12 T g_{\mu\nu})\,w^{\mu}w^{\nu}\ge0\) for all \(w\);

  • dominant energy condition (DEC) if WEC holds and, for every \(w\), the flux vector \(-T^{\mu}{}_{\nu}w^{\nu}\) is causal (non-spacelike) and future-directed — energy does not flow faster than light.

WEC implies NEC by continuity as \(w\) tilts to the light cone; SEC also implies NEC the same way, but SEC does not imply WEC. Rests on Definition 44.6.

Proposition 44.37 (Energy conditions for the perfect fluid).

For the perfect fluid Equation (44.19):

ConditionEquivalent inequalities
NEC$\rho c^{2}+p\ge0$
WEC$\rho\ge0$ \ and \ $\rho c^{2}+p\ge0$
SEC$\rho c^{2}+3p\ge0$ \ and \ $\rho c^{2}+p\ge0$
DEC$\rho\ge0$ \ and \ $\abs{p}\le\rho c^{2}$

Rests on Definitions 44.16 and 44.36.

Proof.

Derives Proposition 44.37. Write the observer as \(w^{\mu}=\gamma(u^{\mu}+v^{\mu})\) with \(u_{\mu}v^{\mu}=0\), \(v^{\mu}\) spacelike of norm \(v^{2}<c^{2}\); normalization forces \(\gamma^{2}(c^{2}-v^{2})=c^{2}\), the Lorentz factor of the relative motion, and \(u_{\mu}w^{\mu}=-\gamma c^{2}\). Then from Equation (44.19),

\begin{equation*} T_{\mu\nu}w^{\mu}w^{\nu} = \left(\rho+\tfrac{p}{c^{2}}\right)\gamma^{2}c^{4} - p\,c^{2} = c^{2}\left[\gamma^{2}c^{2}\rho + \left(\gamma^{2}-1\right)p\right]\ep \end{equation*}

Nonnegativity for all \(\gamma\ge1\) is equivalent to the two endpoint conditions \(\gamma=1\) (\(\rho\ge0\)) and \(\gamma\to\infty\) (\(\rho c^{2}+p\ge0\)), since the expression is affine in \(\gamma^{2}\): that is WEC. For a null \(k\), \(T_{\mu\nu}k^{\mu}k^{\nu}=(\rho+p/c^{2})(u_{\mu}k^{\mu})^{2}\) with \(u_{\mu}k^{\mu}\neq0\), giving NEC. For SEC, the trace is \(T=-\rho c^{2}+3p\), and

\begin{equation*} \left(T_{\mu\nu}-\tfrac12 Tg_{\mu\nu}\right)w^{\mu}w^{\nu} = c^{2}\left[\gamma^{2}\left(\rho c^{2}+p\right) + \tfrac12\left(p-\rho c^{2}\right)\right]\ec \end{equation*}

again affine in \(\gamma^{2}\): nonnegative for all \(\gamma\) iff the slope \(\rho c^{2}+p\ge0\) and the value at \(\gamma=1\), \(\tfrac12(\rho c^{2}+3p)\), is nonnegative. For DEC, compute the flux:

\begin{equation*} f^{\mu} = -T^{\mu}{}_{\nu}w^{\nu} = \gamma\left(\rho c^{2}\,u^{\mu} - p\,v^{\mu}\right)\ec\qquad f^{\mu}f_{\mu} = \gamma^{2}\left(-\rho^{2}c^{6} + p^{2}v^{2}\right)\ep \end{equation*}

Causality of \(f\) for every \(v^{2}<c^{2}\) is equivalent to \(p^{2}c^{2}\le\rho^{2}c^{6}\), i.e. \(\abs{p}\le\rho c^{2}\), and future-direction follows from \(f^{\mu}u_{\mu}=-\gamma\rho c^{4}\le0\) when \(\rho\ge0\).

Proposition 44.38 (The electromagnetic field satisfies NEC, WEC, SEC and DEC).

The stress–energy tensor Equation (44.21) satisfies all four conditions of Definition 44.36. Rests on Proposition 44.17 and Definition 44.36.

Proof.

Derives Proposition 44.38. WEC: for any observer, evaluate in that observer's local orthonormal frame; by Proposition 44.17, \(T_{\mu\nu}w^{\mu}w^{\nu}/c^{2}=T_{\hat0\hat0} =\epsilon_{0}E^{2}/2+B^{2}/2\mu_{0}\ge0\), with \(E\), \(B\) the fields that observer measures. NEC follows by continuity. SEC: the tensor is traceless, so the SEC quadratic form equals the WEC form. DEC: in the observer's frame the flux components are \(f^{\hat0}=c\,T^{\hat0\hat0}=cu\) and \(f^{\hat\imath}=c\,T^{\hat\imath\hat0}=S^{\hat\imath}\), where \(u\) is the energy density above and \(\vect{S}=\vect{E}\times\vect{B}/\mu_{0}\) is the Poynting flux (The Maxwell Equations); causality of \(f\) is \(c^{2}u^{2}\ge\abs{\vect{S}}^{2}\). With \(a=\epsilon_{0}E^{2}\), \(b=B^{2}/\mu_{0}\),

\begin{equation*} u^{2}-\frac{\abs{\vect{S}}^{2}}{c^{2}} = \frac{(a+b)^{2}}{4} - \frac{\epsilon_{0}}{\mu_{0}}\abs{\vect{E}\times\vect{B}}^{2} \ge \frac{(a+b)^{2}}{4} - ab = \frac{(a-b)^{2}}{4}\ \ge\ 0\ec \end{equation*}

using \(\abs{\vect{E}\times\vect{B}}\le\abs{\vect{E}}\abs{\vect{B}}\) and \(\epsilon_{0}/\mu_{0}\cdot E^{2}B^{2}=ab\). Future-direction is \(f^{\hat0}=cu\ge0\).

Proposition 44.39 (SEC is the attraction condition).

Assume the field equations Equation (44.34). Then for every timelike \(w\),

\begin{equation}\tag{44.38} R_{\mu\nu}w^{\mu}w^{\nu} = \kappa\left(T_{\mu\nu} -\tfrac12 T g_{\mu\nu}\right)w^{\mu}w^{\nu} - \Lambda c^{2}\ec \end{equation}

so with \(\Lambda=0\) the SEC is exactly the timelike convergence condition \(R_{\mu\nu}w^{\mu}w^{\nu}\ge0\): through the geodesic deviation equation Equation (43.3), matter satisfying the SEC focuses congruences of free-falling worldlines — gravity attracts. This is the geometric hypothesis under which the singularity theorems of Penrose and of Hawking–Penrose operate [Penrose:1965] [Hawking:1970] [Hawking:1973] (Section 45.4.2); the null convergence condition used in Penrose's theorem follows the same way from the NEC, with the \(\Lambda\) term dropping out on null vectors. Rests on Proposition 44.4 and Definition 44.36.

Proof.

Derives Proposition 44.39. Trace-reverse Equation (44.34) as in Proposition 44.4: tracing gives \(-R+4\Lambda=\kappa T\), so \(R_{\mu\nu}=\kappa(T_{\mu\nu}-\tfrac12 g_{\mu\nu}T) +\Lambda g_{\mu\nu}\), and contracting twice with \(w\) (using \(g_{\mu\nu}w^{\mu}w^{\nu}=-c^{2}\)) gives Equation (44.38). For a null vector the \(g_{\mu\nu}\) terms contract to zero, leaving \(R_{\mu\nu}k^{\mu}k^{\nu}=\kappa T_{\mu\nu}k^{\mu}k^{\nu}\).

Remark 44.40 (The measured universe violates the SEC).

A positive cosmological constant, read as vacuum matter with \(p=-\rho_{\Lambda}c^{2}\) (Remark 44.32), has \(\rho c^{2}+3p=-2\rho_{\Lambda}c^{2}<0\): it violates the SEC while satisfying NEC, WEC and DEC (marginally, at the \(\abs{p}=\rho c^{2}\) boundary). The observed accelerating expansion [Riess:1998] [Perlmutter:1999] is precisely the statement that the SEC fails for the universe's present energy budget (Phenomenon 48.17, Section 48.6): cosmic repulsion is measured, not hypothesized. The SEC therefore has the status of a classical-matter hypothesis, valid for the fluids and fields of Section 44.2.1, appropriate to the collapse and black-hole settings of Schwarzschild Geometry and Black Holes — not a law of nature. The NEC, by contrast, holds for every matter model in this book, and the modern singularity and area theorems lean on it wherever possible.

The initial-value problem

General covariance hides the causal structure of the field equations: ten equations for ten \(g_{\mu\nu}\), but four identities (Remark 44.25) and four coordinate freedoms. The honest count — what data on a spacelike surface determine the future, and through what evolution equations — is the subject of this section. It is also what makes the theory predictive, numerical relativity possible, and the waveform science of Experiment: Gravitational Waves more than curve fitting.

Constraints and evolution

Proposition 44.41 (Four of the ten equations are constraints).

In any coordinates in which \(x^{0}\) is a time function, the four components \(G^{0\nu}\) of the Einstein tensor contain no second \(x^{0}\)-derivative of the metric. The four field equations \(G^{0\nu}=\kappa T^{0\nu}\) are therefore not evolution equations but constraints on the data induced on each surface \(x^{0}=\text{const}\). Rests on Theorem 44.23.

Proof.

Derives Proposition 44.41. The contracted Bianchi identity Equation (44.25), written out,

\begin{equation*} \pp_{0}G^{0\nu} = -\,\pp_{i}G^{i\nu} - \Gamma^{\mu}{}_{\mu\lambda}G^{\lambda\nu} - \Gamma^{\nu}{}_{\mu\lambda}G^{\mu\lambda}\ec \end{equation*}

holds identically in the metric. Every term on the right contains at most second \(x^{0}\)-derivatives of \(g_{\mu\nu}\) (\(G\) is second order and \(\pp_{i}\), \(\Gamma\) add no time derivative). If \(G^{0\nu}\) contained a second time derivative, say a term \(A\,\pp_{0}^{2}g_{\alpha\beta}\) with \(A\) built from lower-order quantities, the left side would contain the third derivative \(A\,\pp_{0}^{3}g_{\alpha\beta}\), which nothing on the right can supply; since the identity holds for every metric, the coefficient \(A\) vanishes identically.

Theorem 44.42 (The constraint equations).

Let \(\Sigma\) be a spacelike hypersurface with future-directed unit normal \(n^{\mu}\) (\(n^{\mu}n_{\mu}=-1\)), induced Riemannian metric \(h_{ij}\), and extrinsic curvature \(K_{\mu\nu}=h^{\alpha}{}_{\mu}h^{\beta}{}_{\nu}\nabla_{\alpha}n_{\beta}\), where \(h^{\alpha}{}_{\mu}=\delta^{\alpha}{}_{\mu}+n^{\alpha}n_{\mu}\) projects onto \(\Sigma\). Write \({}^{(3)}\!R\) for the Ricci scalar of \(h_{ij}\), \(D_{i}\) for its Levi-Civita connection, and \(K=h^{ij}K_{ij}\). Then the normal–normal and normal–tangential projections of the field equations Equation (44.2) read

\begin{align} {}^{(3)}\!R + K^{2} - K_{ij}K^{ij} &= 2\kappa\,T_{\mu\nu}n^{\mu}n^{\nu}\ec \tag{44.39}\\ D_{j}\left(K^{j}{}_{i} - \delta^{j}{}_{i}\,K\right) &= \kappa\,T_{\mu\nu}\,n^{\mu}h^{\nu}{}_{i}\ec \tag{44.40} \end{align}

the Hamiltonian and momentum constraints: equations on the data \((h_{ij},K_{ij})\) alone, with \(T_{\mu\nu}n^{\mu}n^{\nu}\) the energy density and \(-T_{\mu\nu}n^{\mu}h^{\nu}{}_{i}\) the momentum density measured by the observers at rest in \(\Sigma\). Rests on Lemma A.628, Lemma A.630 and Postulate 44.3.

Proof.

Derives Theorem 44.42. The geometric identities are the Gauss and Codazzi equations, proved for arbitrary signature in Appendix A.52 with the normalization \(\epsilon=n^{\mu}n_{\mu}\) carried as a symbol; in this chapter's signature a spacelike surface has \(\epsilon=-1\) and the induced metric \(\gamma_{\mu\nu}=g_{\mu\nu}-\epsilon n_{\mu}n_{\nu}\) used there is our positive-definite \(h_{\mu\nu}\).

Hamiltonian constraint. Contract the Gauss equation Equation (A.985) over its first and third indices, then trace with \(h^{\nu\mu}\). The intrinsic side gives \({}^{(3)}\!R\). The quadratic terms give \(-\epsilon(K_{\mu\nu}K^{\mu\nu}-K^{2})\). The ambient side is the double \(h\)-trace of the projected Riemann tensor; expanding \(h^{\mu\nu}=g^{\mu\nu}+n^{\mu}n^{\nu}\) in both traces and using the Riemann symmetries, the \(nnnn\) term vanishes by antisymmetry, and

\begin{equation*} h^{\alpha\lambda}h^{\tau\sigma}R_{\alpha\tau\lambda\sigma} = R + 2R_{\mu\nu}n^{\mu}n^{\nu}\ep \end{equation*}

Hence, at \(\epsilon=-1\), \({}^{(3)}\!R =R+2R_{\mu\nu}n^{\mu}n^{\nu} +K_{\mu\nu}K^{\mu\nu}-K^{2}\). But \(2G_{\mu\nu}n^{\mu}n^{\nu} =2R_{\mu\nu}n^{\mu}n^{\nu}+R\) since \(g_{\mu\nu}n^{\mu}n^{\nu}=-1\), so

\begin{equation*} {}^{(3)}\!R + K^{2} - K_{ij}K^{ij} = 2\,G_{\mu\nu}n^{\mu}n^{\nu}\ec \end{equation*}

and the field equations replace \(G_{nn}\) by \(\kappa T_{nn}\), giving Equation (44.39).

Momentum constraint. The contracted Codazzi equation Equation (A.990) is \(D_{\nu}(K^{\nu}{}_{\mu}-K\,h^{\nu}{}_{\mu}) =h^{\alpha}{}_{\mu}R_{\alpha\kappa}n^{\kappa}\), with no factor of \(\epsilon\). Since \(h^{\alpha}{}_{\mu}g_{\alpha\kappa}n^{\kappa} =h^{\alpha}{}_{\mu}n_{\alpha}=0\), the Ricci tensor may be replaced by the Einstein tensor, and the field equations by \(\kappa T\); restricting the free index to \(\Sigma\) gives Equation (44.40).

That these are the four equations of Proposition 44.41 follows because \(G_{\mu\nu}n^{\nu}\) and \(G^{0\nu}\) span the same four combinations: \(n_{\mu}\propto\pp_{\mu}x^{0}\) on the surface. Neither Equation (44.39) nor Equation (44.40) contains a time derivative of \(K_{ij}\), i.e. a second time derivative of \(h_{ij}\): they restrict the initial data.

Remark 44.43 (The constrained-Hamiltonian reading, and the count of degrees of freedom).

The same split is the backbone of the canonical formulation worked out, as constrained dynamics, in Section 26.6.5: there the lapse and shift appear as multipliers, the vacuum forms of Equations (44.39) and (44.40) are the secondary constraints \(\Ham_{\perp}\approx0\), \(\Ham_{i}\approx0\) of Theorem 26.42 (stated in the mostly-minus convention; the dictionary is the \(\epsilon\) bookkeeping of Appendix A.52), all eight constraints are first class with the hypersurface-deformation algebra Proposition 26.43, and the count \(2\times10-2\times8=4\) leaves two configuration degrees of freedom per point of space — the two gravitational-wave polarizations of Section 46.2, with no linearization anywhere in the argument. Given constraint-satisfying data, the remaining six field equations evolve \((h_{ij},K_{ij})\) once a lapse and shift — pure gauge — are chosen. Solving the constraints themselves is a nontrivial elliptic problem; the standard method, York's conformal technique, is [York:1972]. And the constraints, once solved, stay solved: Theorem 44.45 below includes the propagation statement, whose engine is again the contracted Bianchi identity.

Well-posedness

That the remaining equations really do evolve the data — existence, uniqueness, continuous dependence, the Hadamard well-posedness of Definition 10.24 — is not visible until the coordinate freedom is fixed, and the fixing that works is the harmonic (de Donder) gauge.

Proposition 44.44 (Harmonic-gauge reduction).

Define \(\Gamma^{\alpha}=g^{\mu\nu}\Gamma^{\alpha}{}_{\mu\nu}\) and \(\Gamma_{\nu}=g_{\nu\alpha}\Gamma^{\alpha}\). Then, identically,

\begin{equation}\tag{44.41} R_{\mu\nu} = -\tfrac{1}{2}\,g^{\lambda\rho}\, \pp_{\lambda}\pp_{\rho}\,g_{\mu\nu} + \tfrac{1}{2}\left(\pp_{\mu}\Gamma_{\nu} + \pp_{\nu}\Gamma_{\mu}\right) + Q_{\mu\nu}\!\left(g,\pp g\right)\ec \end{equation}

where \(Q_{\mu\nu}\) is a polynomial in \(g^{\alpha\beta}\) and \(\pp_{\gamma}g_{\alpha\beta}\), quadratic in the first derivatives, containing no second derivative. In harmonic coordinates — coordinates each satisfying the curved wave equation, equivalently \(\Gamma^{\alpha}=0\) — the vacuum equations \(R_{\mu\nu}=0\) become the reduced equations

\begin{equation}\tag{44.42} g^{\lambda\rho}\,\pp_{\lambda}\pp_{\rho}\,g_{\mu\nu} = 2\,Q_{\mu\nu}\!\left(g,\pp g\right)\ec \end{equation}

ten quasilinear wave equations with a common principal part, the curved d'Alembertian, acting on each component separately. Rests on Theorems 13.150 and 13.152.

Proof.

Derives Proposition 44.44. Only the terms of \(R_{\mu\nu}\) carrying second derivatives need tracking; everything else is by definition collected in \(Q_{\mu\nu}\). From the Ricci contraction of Equation (13.306), \(R_{\mu\nu}=\pp_{\lambda}\Gamma^{\lambda}{}_{\nu\mu} -\pp_{\nu}\Gamma^{\lambda}{}_{\lambda\mu}+\Gamma\Gamma\), and the Christoffel formula, the second-derivative content is

\begin{equation*} R_{\mu\nu} \;\simeq\; \tfrac12 g^{\lambda\sigma}\left( \pp_{\lambda}\pp_{\mu}g_{\sigma\nu} + \pp_{\lambda}\pp_{\nu}g_{\sigma\mu} - \pp_{\lambda}\pp_{\sigma}g_{\mu\nu} - \pp_{\mu}\pp_{\nu}g_{\lambda\sigma}\right)\ec \end{equation*}

\(\simeq\) denoting equality modulo first-derivative terms. On the other hand \(\Gamma_{\nu}\simeq g^{\lambda\sigma}(\pp_{\lambda}g_{\sigma\nu} -\tfrac12\pp_{\nu}g_{\lambda\sigma})\) up to products \((\pp g)(g)\), so

\begin{equation*} \tfrac12\left(\pp_{\mu}\Gamma_{\nu}+\pp_{\nu}\Gamma_{\mu}\right) \;\simeq\; \tfrac12 g^{\lambda\sigma}\left( \pp_{\lambda}\pp_{\mu}g_{\sigma\nu} + \pp_{\lambda}\pp_{\nu}g_{\sigma\mu} - \pp_{\mu}\pp_{\nu}g_{\lambda\sigma}\right)\ep \end{equation*}

Subtracting reproduces exactly the missing \(-\tfrac12 g^{\lambda\sigma}\pp_{\lambda}\pp_{\sigma}g_{\mu\nu}\), which is Equation (44.41). A coordinate function \(x^{\alpha}\) satisfies \(\Box_{g}x^{\alpha} =g^{\mu\nu}\nabla_{\mu}\nabla_{\nu}x^{\alpha} =-g^{\mu\nu}\Gamma^{\alpha}{}_{\mu\nu}=-\Gamma^{\alpha}\), so harmonicity of all four coordinates is \(\Gamma^{\alpha}=0\), and Equation (44.42) follows.

The reduced equations are hyperbolic wherever the metric is Lorentzian, and for analytic data the Cauchy–Kovalevskaya theorem (Theorem 10.22) already yields local solutions. Analyticity, however, is poison for relativity — analytic continuation propagates data instantaneously, defeating the causal structure the equations exist to express — and the honest function spaces are Sobolev, where the machinery is energy estimates for quasilinear hyperbolic systems. That machinery lies beyond this treatise, and the two theorems that close the problem are imported.

Theorem 44.45 (Local existence and uniqueness; Choquet-Bruhat; imported).

Let \((\Sigma,h_{ij},K_{ij})\) be smooth initial data satisfying the vacuum constraints (Equations (44.39) and (44.40) with \(T_{\mu\nu}=0\)). Then there exists a vacuum spacetime \((M,g_{\mu\nu})\) — a development of the data — containing an embedded hypersurface with induced metric \(h_{ij}\) and extrinsic curvature \(K_{ij}\), obtained by solving the reduced equations Equation (44.42); the harmonic gauge condition and the constraints, imposed at the initial surface, propagate; and any two developments agree, near \(\Sigma\), up to a diffeomorphism fixing \(\Sigma\). The Cauchy problem of general relativity is well posed in the sense of Definition 10.24 [ChoquetBruhat:1952]. Rests on Theorem 44.42, Proposition 44.44 and Definition 10.24.

Theorem 44.46 (Maximal globally hyperbolic development; Choquet-Bruhat and Geroch; imported).

Among all globally hyperbolic vacuum developments of given constraint-satisfying data there is a maximal one, unique up to isometry, into which every other embeds isometrically [ChoquetBruhat:1969]. Rests on Theorems 44.42 and 44.45.

Remark 44.47 (Status of the imports, and what hangs on them).

Theorem 44.45 is Choquet-Bruhat's 1952 theorem, published under the name Fourès-Bruhat [ChoquetBruhat:1952]; modern proofs, with the Sobolev thresholds and the constraint-propagation computation written out, are in [Wald:1984] (ch. 10) and [Hawking:1973] (ch. 7). The propagation argument is worth stating even unproved, because it closes this chapter's circle: if the reduced equations hold, the contracted Bianchi identity Equation (44.25) forces the four quantities \(\Gamma^{\alpha}\) to satisfy a linear homogeneous hyperbolic system; data satisfying the constraints start the \(\Gamma^{\alpha}\) and their first time derivatives at zero; and the unique solution of a homogeneous system with zero data is zero — so the gauge condition maintains itself and the reduced solution solves the full Einstein equations. Theorem 44.46 then removes the arbitrariness of gauge and extent in one stroke: general relativity assigns to each admissible initial datum a unique maximal spacetime. Determinism holds exactly as far as global hyperbolicity does; whether it can fail beyond — Cauchy horizons, naked singularities — is the cosmic-censorship question of Section 45.4.3 [Penrose:1969]. On these two theorems rests numerical relativity: well-posedness is what guarantees that discretized evolutions converge to the continuum solution, and with it the template waveforms against which the detections of Experiment: Gravitational Waves are read.

Exact solutions: an overview

The field equations are ten coupled quasilinear PDEs, and their generic solution is numerical. The exactly solved cases are few, each purchased with heavy symmetry, and almost every observational confrontation in this part runs through one of them. They are collected here once, with their working homes; each named solution is derived in the chapter that consumes it.

The exact solutions this treatise uses. Each is derived and exploited in the chapter of the last column; the citations for the original papers are given in the text below.

SolutionSymmetrySourceTreated in
Minkowskimaximal, flatvacuumMinkowski Space and Its Symmetries
de Sitter / anti-de Sittermaximal$\Lambda$ onlySection 44.6
Schwarzschild exteriorstatic, sphericalvacuumSchwarzschild Geometry and Black Holes
Interior fluid spheresstatic, sphericalperfect fluidCompact Stars and Relativistic Astrophysics
Kerrstationary, axialvacuumSchwarzschild Geometry and Black Holes
FLRW cosmologieshomogeneous, isotropicperfect fluidEvidence-Based Cosmology
Oppenheimer–Snyderspherical, dynamicaldustSchwarzschild Geometry and Black Holes
Linearized wavesnone (perturbative)weak sourcesGravitational-Wave Theory

The Schwarzschild exterior solution — found within weeks of the field equations, from the trenches of the eastern front — describes the vacuum outside any spherical mass [Schwarzschild:1916], with Droste's independent derivation arriving months later in the now-standard coordinates [Droste:1917]; by Birkhoff's theorem (Section 45.1.2) it is the unique spherically symmetric vacuum solution, static or not. It underwrites the classical tests (Experiment: The Classical Tests of General Relativity) and, continued inside its horizon, the black hole (Schwarzschild Geometry and Black Holes). Its interior companions — Schwarzschild's constant-density sphere and the Tolman–Oppenheimer–Volkoff hydrostatics built on Equation (44.24) — carry relativistic stellar structure [Tolman:1939] [Oppenheimer:1939a] and are the business of Compact Stars and Relativistic Astrophysics; the Oppenheimer–Snyder collapse of a dust ball [Oppenheimer:1939b] is the exactly solvable model of black-hole formation (Section 45.4.1). The Kerr solution, the stationary rotating vacuum found only in 1963 [Kerr:1963], is by the no-hair theorems (Section 45.5.3) the endpoint of every gravitational collapse and the metric read directly by the observations of Experiment: Black-Hole Observations. The Friedmann–Lemaître–Robertson–Walker family — Friedmann's dynamical solutions [Friedmann:1922], Lemaître's independent expansion physics [Lemaitre:1927], and the Robertson–Walker proof that the metric form is forced by homogeneity and isotropy alone [Robertson:1935] [Walker:1937] — instantiates the maximally symmetric spaces of Section 13.13 as the spatial sections of cosmology, and carries all of Evidence-Based Cosmology. Plane gravitational waves close the list (Gravitational-Wave Theory). The systematic monographs are [Misner:1973] [Wald:1984].

What the short list teaches is the shape of the subject: a handful of exact geometries, each pinned to data — planetary orbits and light bending for Schwarzschild, X-ray binaries, stellar dynamics and horizon-scale imaging for Kerr, the expansion history for FLRW, interferometer strain for the waves — with the equations themselves, checked in Section 44.4.2 against the Newtonian world and secured as a well-posed dynamical system in Section 44.9, mediating between them. The chapters that follow take up each geometry in turn.