Numerical evolution of relativistic hydrodynamics has been traditionally carried out on spacelike Cauchy hypersurfaces. Although the Bondi–Sachs evolution algorithm can easily be extended to include matter [153], the advantage of a light cone approach for treating fluids is not as apparent as for a massless field whose physical characteristics lie on the light cone. However, results from recent studies of relativistic stars and of fluid sources moving in the vicinity of a black hole indicate that this approach can provide accurate simulations of astrophysical relevance such as supernova collapse to a black hole, mass accretion, and the production of gravitational waves.

7.1 Spherically symmetric hydrodynamic codes

7.2 Axisymmetric characteristic hydrodynamic simulations

7.3 Three-dimensional characteristic hydrodynamic simulations

7.3.1 Massive particle orbiting a black hole

7.2 Axisymmetric characteristic hydrodynamic simulations

7.3 Three-dimensional characteristic hydrodynamic simulations

7.3.1 Massive particle orbiting a black hole

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