Gravitational Radiation from Coalescing Binary Neutron Stars. I

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Abstract
We have performed numerical simulations of coalescence of a binary system consisting of two neutron stars using a Newtonian hydrodynamics code, which is constructed adopting LeBlanc’s method for a transport term with tensor artificial viscosity terms to express shock waves. We use a Cartesian coordinate system (x, y, z) and take typically a 141 ×141 ×141 grid. The code passed various test-bed problems. Calculation is started when two neutron stars just contact with each other. We use a polytropic equation of state with γ=2 to express high density matter and the amount of gravitational waves is estimated using a quadrupole formula. For the coalescence of two neutron stars of each mass 1.4 M⊙, the total energy radiated during the first 1.9 msec can be 2.7 % of the 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 simulation including the back reaction is urgent to know the final destiny. Wave patterns as well as energy spectra of gravitational waves are also shown.

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