Titlebook: Relativity and Scientific Computing; Computer Algebra, Nu Friedrich W. Hehl,Roland A. Puntigam,Hanns Ruder Book 1996 Springer-Verlag Berlin

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Numerical Relativity and Black-Hole Collisionse initial-data sets and their construction, coordinate choices for the initial data and evolution, boundary conditions and apparent horizon techniques, event-horizon finders and applications, and recent progress in this area.

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Temporal and Spatial Foliations of Spacetimesby 2-surfaces of .. Apart from the equations for the shift vector, which can be derived for this gauge condition, we have investigated such spatial foliations for well-known stationary axially symmetric spacetimes, namely for the Kerr metric and for numerically determined solutions for rapidly rotating neutron stars.

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Numerical Relativity and Black-Hole Collisionses. There are two parts to the lectures: (1) numerical relativity and parallel computing, and (2) evolving black-hole spacetimes. In the first part, I describe the astrophysical motivation behind this work, the formulation of the equations for numerical relativity, slicing and gauge conditions, nume

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Four Lectures on Numerical Relativitych is shown to be hyperbolic when the time coordinate is chosen in an invariant algebraic way (maximal slicing is recovered as a limiting case). The second lecture deals with first-order flux-conservative systems. The propagation of characteristic fields in an inhomogeneous background is also consid

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Alternatives to Finite Difference Methods in Numerical Relativitychallenge effort in the United States to simulate, by the end of the century, black-hole collisions is entirely based on finite difference codes. Furthermore, the power of finite difference techniques has recently been enhanced with the implementation of adaptive mesh refinements. In spite of the fi

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Rotating and Oscillating Neutron Starse and gravitational fields of spherically symmetric, nonrotating stars are governed by the Tolman-Oppenheimer-Volkoff equations, a set of ordinary differential equations. The determination of solutions for . stars is a much more complicated numerical problem, because in this case a system of . diffe

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Rotating Boson Starsnstruct for the first time the corresponding localized rotating configurations via numerical integration of the coupled Einstein-Klein-Gordon equations. The ratio of conserved angular momentum and particle number turns out to be an integer ., the . of our soliton-type stars. The resulting axisymmetr