A perturbative approach to the numerical simulation of rotational collapse of neutron stars

Details A perturbative approach to the numerical simulation of rotational collapse of neutron stars A perturbative approach to the numerical simulation of rotational collapse of neutron stars

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..apr.u9002s&link_type=abstract

American Physical Society, April Meeting, 2003, April 5-8, 2003 Philadelphia, Pennsylvania, MEETING ID: APR03, abstract #U9.002

Physics

Scientific paper

The collapse of rotating stars/stellar cores has attracted a lot of attention in the past and is considered among the most promising sources of detectable gravitational waves. We approach the numerical simulation of such scenarios in the slow rotation approximation by evolving gauge invariant second order perturbations on the background of a spherically symmetric collapsing neutron star. Our project thus represents a generalization to 'neutron stars with barotropic equations of state' of work by Cunningham, Price and Moncrief who applied this idea to the analytic background solution for Oppenheimer-Snyder dust collapse. In the slow rotation approximation this approach enables us to obtain fully relativistic simulations of rotating collapsing stars within a well understood numerical framework.

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