Evolution of Close Neutron Star Binaries

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Abstract
We have calculated the evolution of neutron star binaries towards the coalescence driven by gravitational radiation. The hydrodynamical effects as well as the general relativistic effects are important in the final phase. All corrections up to post*-Newtonian order and the tidal effect are included in the orbital motion. The star is approximated using a simple Newtonian stellar model called the affine star model. Stellar spins and angular momentum are assumed to be aligned. We have shown how the internal stellar structure affects the stellar deformation, variations of the spins, and the orbital motion of the binary just before contact. The gravitational wave, radiated from the last few revolutions, significantly depends on the stellar structure.

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