2000/12/04 by Jonathan Thornburg, Thornburg, Jonathan
Physics and Astronomy · #Advanced X-ray Imaging Techniques #Astrophysical Phenomena and Observations #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #Pulsars and Gravitational Waves Research #gr-qc
paper · pdf · doi:10.48550/arxiv.gr-qc/0012012
LaTeX, 2 pages including 1 postscript figure; uses World Scientific style file ws-p9-75x6-50.cls (enclosed); to appear in Proceedings of the 9th Marcel Grossman Meeting; talk presented 6 July 2000 in MG9 session CM3 - Black Hole Collisions
arxiv created 2000/12/04 · openalex publication_date 2000/12/04 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
When using black hole excision to numerically evolve a fully generic black hole spacetime, most 3-D 3+1 codes use an xyz-topology (spatial) grid. In such a grid, an r = \constant excision surface must be approximated by an irregular and non-smooth "staircase-shaped" excision grid boundary, which may introduce numerical instabilities into the evolution. In this paper I describe an alternate scheme, which uses multiple grid patches, each with topology \r × (\rm angular coordinates)\, to cover the slice outside the r = \constant excision surface. The excision grid boundary is now smooth, so the evolution should be less prone to instabilities. With 4th order finite differencing, this code evolves Kerr initial data to ∼ 60M using the ADM equations; I'm currently implementing the BSSN equations in it in the hope that this will improve the stability.