Treating Numerical Instabilities in Irrotational Binary Neutron Star Coalescence Calculations

Details Treating Numerical Instabilities in Irrotational Binary Neutron Star Coalescence Calculations Treating Numerical Instabilities in Irrotational Binary Neutron Star Coalescence Calculations

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aps..dcm.c3002f&link_type=abstract

American Physical Society, DCOMP Meeting, June 25-28, 2001 Cambridge, Massachusetts Bulletin of the American Physical Society, V

Physics

Scientific paper

The final burst of gravitational radiation emitted by coalescing binary neutron stars carries direct information about the neutron star fluid, and, in particular, about the equation of state of nuclear matter at extreme densities. Here, we present results from our latest post-Newtonian SPH calculations of binary neutron star coalescence, using up to 10^6 SPH particles to compute with higher spatial resolution than ever before the merger of an initially irrotational system. We discuss the numerical difficulties associated with instabilities which occur in such calculations, and discuss their effect on predictions of gravity wave signals and spectra.

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