Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..apr.u9001d&link_type=abstract
American Physical Society, April Meeting, 2003, April 5-8, 2003 Philadelphia, Pennsylvania, MEETING ID: APR03, abstract #U9.001
Astronomy and Astrophysics
Astrophysics
Scientific paper
Numerous astrophysical problems involving gravitational collapse, instabilities in rotating relativistic stars, binary neutron star and black hole coalescence, supermassive star collapse, and hypernova core collapse, require three-dimensional numerical modeling in full general relativity for a complete solution. A numerical relativity code must be able to (1) handle the relativistic flows and shocks arising during collapse, (2) deal with any black hole spacetime singularites when they form, and (3) remain sufficiently accurate and stable to evolve a dynamical system until it reaches a quiescent state. We demonstrate the ability of our new relativistic hydrodynamics code to achieve these goals in tackling a variety of astrophysical problems involving strong gravitational fields. For example, we show how our code can model collapse of an unstable, rotating star reliably up to the appearance of an apparent horizon. We then show how we are able to extend the evolution long after a black hole is formed, tracing out the continued in-fall of matter, until the system reaches a stationary state.
Baumgarte Thomas
Duez Matthew
Marronetti Pedro
Shapiro Stuart
Yo Hwei-Jang
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