With respect to an adapted coordinate , so that , the metric of a stationary spacetime can be parameterized in terms of a three-dimensional (Riemannian) metric , a one-form , and a scalar field , where stationarity implies that , and are functions on :
The notation suggests that is a time coordinate, , but this restriction does not play any role in the local form of the equations that we are about to derive. Similarly the local calculations that follow remain valid regardless of the causal character of , provided that is not null everywhere, and then one only considers the region where does not change sign. On any connected component of this region is either spacelike or timelike, as determined by the sign of , and then the metric is Lorentzian, respectively Riemannian, there. In any case, both the parameterization of the metric and the equations become singular at places where has zeros, so special care is required wherever this occurs.
Using Cartan’s structure equations (see, e.g., ), it is a straightforward task to compute the Ricci scalar for the above decomposition of the spacetime metric; see, e.g.,  for the details of the derivation. The result is that the Einstein–Hilbert action of a stationary spacetime reduces to the action for a scalar field and a vector field , which are coupled to three-dimensional gravity. The fact that this coupling is minimal is a consequence of the particular choice of the conformal factor in front of the three-metric in the decomposition (6.1). The vacuum field equations are thus seen to be equivalent to the three-dimensional Einstein-matter equations obtained from variations of the effective action
It is worth noting that the quantities and are related to the norm and the twist of the Killing field as follows:
Living Rev. Relativity 15, (2012), 7
This work is licensed under a Creative Commons License.