  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.
