The NP version [39, 44, 41] of the vacuum Einstein (or the Einstein–Maxwell) equations uses the tetrad components
The complex spin coefficients, which play the role of the connection, are determined from the Ricci rotation coefficients [39, 44]:
The third basic variable in the NP formalism is the Weyl tensor or, equivalently, the following five complex tetrad components of the Weyl tensor:
When an electromagnetic field is present, we must include the complex tetrad components of the Maxwell field into the equations:
Remark: We mention that much of the physical content and interpretations in the present work comes from the study of the lowest spherical harmonic coefficients in the leading terms of the far-field expansions of the Weyl and Maxwell tensors.
The NP version of the vacuum (or Einstein–Maxwell) equations consists of three sets (or four sets) of nonlinear first-order coupled partial differential equations for the variables: the tetrad components, the spin coefficients, the Weyl tensor (and Maxwell field when present). Though there is no hope that they can be solved in any general sense, many exact solutions have been found from them. Of far more importance, large classes of asymptotic solutions and perturbation solutions can be found. Our interest lies in the asymptotic behavior of the asymptotically-flat solutions. Though there are some subtle issues, integration in this class is not difficult [39, 45]. With no explanation of the integration process, except to mention that we use the Bondi coordinate and tetrad system of Equations (7), (9), and (11) and asymptotic flatness, we simply give the final results.
First, the radial behavior is described. The quantities with a zero superscript, e.g., , , …, are ‘functions of integration’, i.e., functions only of ().
Remark: These last five equations, the first of which contains the beautiful Bondi energy-momentum loss theorem, play the fundamental role in the dynamics of our physical quantities.
Remark: Using the mass aspect, , with Equations (51) and (52), the first of the asymptotic Bianchi identities can be rewritten in the concise form,
From these results, the characteristic initial problem can roughly be stated in the following manner. At we choose the initial values for (, i.e., functions only of (). The characteristic data, the complex Bondi shear, , is then freely chosen. Since and are functions of , Equations (49), (51) and (52) and its derivatives, all the asymptotic variables can now be determined from Equations (56) – (60).
An important consequence of the NP formalism is that it allows simple proofs for many geometric theorems. Two important examples are the Goldberg–Sachs theorem  and the peeling theorem . The peeling theorem is essentially given by the asymptotic behavior of the Weyl tensor in Equation (40) (and Equation (41)). The Goldberg–Sachs theorem essentially states that for an algebraically-special metric, the degenerate principle null vector field is the tangent field to a shear-free NGC. Both theorems are implicitly used later.
One of the immediate physical interpretations arising from the asymptotically-flat solutions was Bondi’s  identifications, at , of the interior spacetime four-momentum (energy/momentum). Given the mass aspect, Equation (54),
and the spherical harmonic expansion
The evolution of these quantities, (the Bondi mass/momentum loss) is then determined from Equation (62). The details of this will be discussed in Section 5.
The same clear cut asymptotic physical identification for interior angular momentum is not as readily available. In vacuum linear theory, the angular momentum is often taken to be. In the presence of a Maxwell field, this is again modified by the addition of electromagnetic multipole terms [29, 3].
In our case, where we consider only quadrupole gravitational radiation, the quadratic correction terms do in fact vanish and hence Equation (66), modified by the Maxwell terms, is correct as it is stated.
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