Measurability of the tidal deformability by gravitational waves from coalescing binary neutron stars

Combining new gravitational waveforms derived by long-term (14--16 orbits) numerical-relativity simulations with waveforms by an effective-one-body (EOB) formalism for coalescing binary neutron stars, we construct hybrid waveforms and estimate the measurability for the dimensionless tidal deformability of the neutron stars, $\Lambda$, by advanced gravitational-wave detectors. We focus on the equal-mass case with the total mass $2.7M_\odot$. We find that for an event at a hypothetical effective distance of $D_{\rm eff}=200$ Mpc, the distinguishable difference in the dimensionless tidal deformability will be $\approx 100$, 400, and 800 at 1-$\sigma$, 2-$\sigma$, and 3-$\sigma$ levels, respectively, for advanced LIGO. If the true equation of state is stiff and the typical neutron-star radius is $R \gtrsim 13$ km, our analysis suggests that the radius will be constrained within $\approx 1$ km at 2-$\sigma$ level for an event at $D_{\rm eff}=200$ Mpc. On the other hand, if the true equation of state is soft and the typical neutron-star radius is $R\lesssim 12$ km , it will be difficult to narrow down the equation of state among many soft ones, although it is still possible to discriminate the true one from stiff equations of state with $R\gtrsim 13$ km. We also find that gravitational waves from binary neutron stars will be distinguished from those from spinless binary black holes at more than 2-$\sigma$ level for an event at $D_{\rm eff}=200$ Mpc. The validity of the EOB formalism, Taylor-T4, and Taylor-F2 approximants as the inspiral waveform model is also examined.