Binary neutron stars as sources of gravitational waves

Details Binary neutron stars as sources of gravitational waves Binary neutron stars as sources of gravitational waves

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sf2a.conf..351g&link_type=abstract

SF2A-2004: Semaine de l'Astrophysique Francaise, meeting held in Paris, France, June 14-18, 2004. Edited by F. Combes, D. Barret

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Coalescing neutron star binaries are expected to be among the strongest sources of gravitational radiation to be seen by laser interferometers. Using the well tested StarTrack binary population synthesis code we show that regardless of the maximal mass of a neutron star a significant fraction of the observed systems in gravitational waves will have low mass ratios < 0.7. Taking into account both the above results and properties of the known double neutron star binaries we perform calculations of the final phase of binary neutron star inspiral in general relativity. We show that for neutron star binaries described by modern realistic equation of state (Akmal et al. 1998) the merger will take place for high frequency of gravitational waves > 1.1 kHz regardless of the mass ratio 0.675; 0.9; 1. We discuss the dependence of gravitational waveforms on nuclear equations of state.

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