In general relativity and quantum gravity, the Gibbons–Hawking–York boundary term is a term that needs to be added to the Einstein–Hilbert action when the underlying spacetime manifold has a boundary. The Einstein–Hilbert action is the basis for the most elementary variational principle from which the field equations of general relativity can be defined. However, the use of the Einstein–Hilbert action is appropriate only when the underlying spacetime manifold M {\displaystyle {\mathcal {M}}} is closed, i.e. a manifold which is both compact and without boundary. In the event that the manifold has a boundary ∂ M {\displaystyle \partial {\mathcal {M}}} , the action should be supplemented by a boundary term so that the variational principle is well-defined. The necessity of such a boundary term was first realised by James W. York and later refined in a minor way by Gary Gibbons and Stephen Hawking. For a manifold that is not closed, the appropriate action is
S E H + S G H Y = 1 16 π ∫ M d 4 x − g R + 1 8 π ∫ ∂ M d 3 y ϵ h K , {\displaystyle {\mathcal {S}}_{\mathrm {EH} }+{\mathcal {S}}_{\mathrm {GHY} }={\frac {1}{16\pi }}\int _{\mathcal {M}}\mathrm {d} ^{4}x\,{\sqrt {-g}}R+{\frac {1}{8\pi }}\int _{\partial {\mathcal {M}}}\mathrm {d} ^{3}y\,\epsilon {\sqrt {h}}K,}
where S E H {\displaystyle {\mathcal {S}}_{\mathrm {EH} }} is the Einstein–Hilbert action, S G H Y {\displaystyle {\mathcal {S}}_{\mathrm {GHY} }} is the Gibbons–Hawking–York boundary term, h a b {\displaystyle h_{ab}} is the induced metric (see section below on definitions) on the boundary, h {\displaystyle h} its determinant, K {\displaystyle K} is the trace of the second fundamental form, ϵ {\displaystyle \epsilon } is equal to + 1 {\displaystyle +1} where the normal to ∂ M {\displaystyle \partial {\mathcal {M}}} is spacelike and − 1 {\displaystyle -1} where the normal to ∂ M {\displaystyle \partial {\mathcal {M}}} is timelike, and y a {\displaystyle y^{a}} are the coordinates on the boundary. Varying the action with respect to the metric g α β {\displaystyle g_{\alpha \beta }} , subject to the condition
δ g α β | ∂ M = 0 , {\displaystyle \delta g_{\alpha \beta }{\big |}_{\partial {\mathcal {M}}}=0,}
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