Radiation tails and boundary conditions for black hole evolutions
arXiv:gr-qc/0401092 · doi:10.1103/PhysRevD.70.044038
Abstract
In numerical computations of Einstein's equations for black hole spacetimes, it will be necessary to use approximate boundary conditions at a finite distance from the holes. We point out here that ``tails,'' the inverse power-law decrease of late-time fields, cannot be expected for such computations. We present computational demonstrations and discussions of features of late-time behavior in an evolution with a boundary condition.
submitted to Phys. Rev. D
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