Gravitational Radiation from Coalescing Binary Neutron Stars. I

Details Gravitational Radiation from Coalescing Binary Neutron Stars. I Gravitational Radiation from Coalescing Binary Neutron Stars. I

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989pthph..82..535o&link_type=abstract

Progress of Theoretical Physics, Vol. 82, No. 3, pp. 535-554

Physics

46

Scientific paper

We have performed numerical simulations of coalescence of a binary system consisting of twoneutron stars using a Newtonian hydrodynamics code, which is constructed adopting LeBlanc'smethod for a transport term with tensor artificial viscosity terms to express shock waves. We usea Cartesian coordinate system (x, y, z) and take typically a 141 x 141 x 141 grid. The code passedvarious test-bed problems. Calculation is started when two neutron stars just contact with eachother. We use a polytropic equation of state with gamma=2 to express high density matter and theamount of gravitational waves is estimated using a quadrupole formula. For the coalescence of twoneutron stars of each mass 1.4 Msun, the total energy radiated during the first 1.9 msec can be 2.7 % ofthe rest mass, which is much larger than any estimates of the burst sources of the gravitational waves.The luminosity in the final stage of our calculation is still high. This fact indicates that simulationincluding the back reaction is urgent to know the final destiny. Wave patterns as well as energyspectra of gravitational waves are also shown.

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