  We have calculated 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$^{2.5}$-Newtonian order and the tidal effect are included in the
orbital motion. The star is approximated by a simple Newtonian stellar model
called affine star model. Stellar spins and angular momentum are assumed to be
aligned. We have showed how the internal stellar structure affects the stellar
deformation, variations of the spins, and the orbital motion of the binary just
before the contact. The gravitational wave forms from the last a few
revolutions significantly depend on the stellar structure.
