Thus the metric and the equations of motion for matter become the primary entities for calculating observable effects, and all that distinguishes one metric theory from another is the particular way in which matter and possibly other gravitational fields generate the metric.
The comparison of metric theories of gravity with each other and with experiment becomes particularly simple when one takes the slowmotion, weakfield limit. This approximation, known as the postNewtonian limit, is sufficiently accurate to encompass most solarsystem tests that can be performed in the foreseeable future. It turns out that, in this limit, the spacetime metric predicted by nearly every metric theory of gravity has the same structure. It can be written as an expansion about the Minkowski metric () in terms of dimensionless gravitational potentials of varying degrees of smallness. These potentials are constructed from the matter variables (see Box 2) in imitation of the Newtonian gravitational potential
The “order of smallness” is determined according to the rules , , and so on (we use units in which ; see Box 2).A consistent postNewtonian limit requires determination of correct through , through , and through (for details see TEGP 4.1 [281]). The only way that one metric theory differs from another is in the numerical values of the coefficients that appear in front of the metric potentials. The parametrized postNewtonian (PPN) formalism inserts parameters in place of these coefficients, parameters whose values depend on the theory under study. In the current version of the PPN formalism, summarized in Box 2, ten parameters are used, chosen in such a manner that they measure or indicate general properties of metric theories of gravity (see Table 2). Under reasonable assumptions about the kinds of potentials that can be present at postNewtonian order (basically only Poissonlike potentials), one finds that ten PPN parameters exhaust the possibilities.

The parameters and are the usual Eddington–Robertson–Schiff parameters used to describe the “classical” tests of GR, and are in some sense the most important; they are the only nonzero parameters in GR and scalartensor gravity. The parameter is nonzero in any theory of gravity that predicts preferredlocation effects such as a galaxyinduced anisotropy in the local gravitational constant G_{L} (also called “Whitehead” effects); , , measure whether or not the theory predicts postNewtonian preferredframe effects; , , , , measure whether or not the theory predicts violations of global conservation laws for total momentum. In Table 2 we show the values these parameters take
Semiconservative theories have five free PPN parameters (, , , , ) while fully conservative theories have three (, , ).
The PPN formalism was pioneered by Kenneth Nordtvedt [197], who studied the postNewtonian metric of a system of gravitating point masses, extending earlier work by Eddington, Robertson and Schiff (TEGP 4.2 [281]). Will [274] generalized the framework to perfect fluids. A general and unified version of the PPN formalism was developed by Will and Nordtvedt. The canonical version, with conventions altered to be more in accord with standard textbooks such as [189], is discussed in detail in TEGP 4 [281]. Other versions of the PPN formalism have been developed to deal with point masses with charge, fluid with anisotropic stresses, bodies with strong internal gravity, and postpostNewtonian effects (TEGP 4.2, 14.2 [281]).
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Box 2. The Parametrized PostNewtonian formalism
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