Coalescing Neutron Stars

Details Coalescing Neutron Stars Coalescing Neutron Stars

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.1001d&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #10.01; Bulletin of the American Astronomical Society, Vol. 24, p.1132

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We present 3D Newtonian simulations of the coalescence of two neutron stars, using a Smoothed Particle Hydrodynamics (SPH) code. We begin the simulations with the two stars in a hard, circular binary, and have them spiral together as angular momentum is lost through gravitational radiation at the rate predicted by modeling the system as two point masses. We model the neutron stars as hard polytropes (gamma =2.4) of equal mass, and investigate the effect of the initial spin of the two stars on the coalescence. The process of coalescence, from initial contact to the formation of an axially symmetric object, takes only a few orbital periods. We follow the emission of gravitional radiation assuming the quadrupole approximation. Such merging binaries will be an important source of gravitational radiation for the Laser Interferometer Gravitational-Wave Observatory (LIGO), as well as providing a possible candidate for gamma -ray bursts if they occur at cosmological distances.

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