Eulderink and Mellema [115, 117] were the first to derive a covariant formulation of the GRHD equations. As in the formulation discussed in Section 2.1.3, these authors took special care to use the conservative form of the system, with no derivatives of the dependent fluid variables appearing in the source terms. Additionally, this formulation is strongly adapted to a particular numerical method based upon a generalization of Roe’s approximate Riemann solver. Such a solver was first applied to the nonrelativistic Euler equations in  and has been widely employed since in simulating compressible flows in computational fluid dynamics. Furthermore, their procedure is specialized for a perfect-fluid EOS, , being the (constant) adiabatic index of the fluid.
After the appropriate choice of the state-vector variables, the conservation laws, Equations (7) and (8), are rewritten in flux-conservative form. The flow variables are then expressed in terms of a parameter vector as
Eulderink and Mellema computed the exact “Roe matrix”  for the vector (38) and obtained the corresponding spectral decomposition. The characteristic information is used to solve the system numerically using Roe’s generalized approximate Riemann solver. Roe’s linearization can be expressed in terms of the average state[115, 117].
The performance of this general-relativistic Roe solver was tested in a number of one-dimensional problems for which exact solutions are known, including nonrelativistic shock tubes, special-relativistic shock tubes, and the spherical accretion of dust and a perfect fluid onto a (static) Schwarzschild black hole. In its special-relativistic version it has been used in the study of the confinement properties of relativistic jets . However, no astrophysical applications in strong-field general-relativistic flows have yet been attempted with this formulation.
In this formulation , the spatial velocity components of the 4-velocity, , together with the rest-frame density and internal energy, and , provide a unique description of the state of the fluid at a given time and are taken as the primitive variables. They constitute a vector in a five-dimensional space . The initial-value problem for Equations (7) and (8) is defined in terms of another vector in the same fluid-state space, namely the conserved variables, , individually denoted :
The flux vectors and the source terms (which depend only on the metric, its derivatives, and the undifferentiated stress-energy tensor), are given by
The state of the fluid is uniquely described using either vector of variables, i.e., either or , and each one can be obtained from the other via the definitions (40) – (42) and the use of the normalization condition for the 4-velocity, . The local characteristic structure of the above system of equations was presented in , where the formulation proved well suited for the numerical implementation of HRSC schemes. The formulation of  was developed for a perfect fluid EOS. Extensions to account for generic EOS are given in , where a comprehensive analysis of general-relativistic hydrodynamics in conservation form is also provided.
A technical remark must be included here. In all conservative formulations discussed in Sections 2.1.3, 2.2.1, and 2.2.2, the time update of a given numerical algorithm is applied to the conserved quantities . After this update the vector of primitive quantities must be reevaluated, as those are needed in the Riemann solver (see Section 4.1.2). The relation between the two sets of variables is, in general, not in closed form and, hence, the recovery of the primitive variables is done using a root-finding procedure, typically a Newton–Raphson algorithm. This feature, distinctive of the equations of (special and) general-relativistic hydrodynamics – it does not exist in the Newtonian limit – may lead, in some cases, to accuracy losses in regions of low density and small speeds, apart from being computationally inefficient. The specific details of this issue for each formulation of the equations can be found in [36, 117, 311]. In particular, for the covariant formulation discussed in Section 2.2.1, there exists an analytic method to determine the primitive variables, which is, however, computationally very expensive since it involves many extra variables and the solving of a quartic polynomial. Therefore, iterative methods are still preferred . On the other hand, we note that the covariant formulation discussed in this section, when applied to null-spacetime foliations, allows for a simple and explicit recovery of the primitive variables, as a consequence of the particular form of the Bondi–Sachs metric.
The general formalism laid out in [311, 309] has been applied to astrophysical problems of increasing complexity. Applications in spherical symmetry include the investigation of accreting dynamic black holes, which can be found in [311, 312]. Studies of the gravitational collapse of supermassive stars are discussed in  and studies of the interaction of scalar fields with relativistic stars are presented in . Axisymmetric neutron-star spacetimes are considered in , and results for axisymmetric gravitational-core collapse using characteristic numerical relativity can be found in . A proof-of-principle demonstration of the inclusion of matter fields in three dimensions was first given in and short-time evolutions of a self-gravitating star in close orbit around a black hole have only been accomplished recently .
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