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We present numerical results of three-dimensional simulations for the mergerof binary neutron stars (BNSs) in full general relativity. Hybrid equations ofstate (EOSs) are adopted to mimic realistic nuclear EOSs. In this approach, wedivide the EOSs into two parts, i.e., the thermal part and the cold part. Forthe cold part, we assign a fitting formula for realistic EOSs of cold nuclearmatter slightly modifying the formula developed by Haensel and Potekhin. Weadopt the SLy and FPS EOSs for which the maximum allowed ADM mass of cold andspherical neutron stars (NSs) is ~ 2.04Mo and 1.80Mo, respectively. Simulationsare performed for BNSs of the total ADM mass in the range between 2.4Mo and2.8Mo with the rest-mass ratio Q_M to be in the range 0.9 < Q_M < 1. It isfound that if the total ADM mass of the system is larger than a thresholdM_{thr}, a black hole (BH) is promptly formed in the merger irrespective of themass ratios. In the other case, the outcome is a hypermassive NS of a largeellipticity, which results from the large adiabatic index of the realistic EOSsadopted. The value of M_{thr} depends on the EOS: ~ 2.7Mo and ~ 2.5Mo for theSLy and FPS EOSs, respectively. Gravitational waves are computed in terms of agauge-invariant wave extraction technique. In the formation of the hypermassiveNS, quasiperiodic gravitational waves of a large amplitude and of frequencybetween 3 and 4 kHz are emitted. The estimated emission time scale is < 100 ms,after which the hypermassive NS collapses to a BH. Because of the long emissiontime, the effective amplitude may be large enough to be detected by advancedlaser interferometric gravitational wave detectors if the distance to thesource is smaller than ~ 100 Mpc.Comment: Typos corrected, 2 references and comments on them added, 26 pages,  54 Postscript figures, Phys.Rev.D in pres

Merger of binary neutron stars with realistic equations of state in full general relativity