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We calculate quasiequilibrium sequences of equal-mass, irrotational binaryneutron stars (BNSs) in a scalar-tensor (ST) theory of gravity that admitsdynamical scalarization. We model neutron stars with realistic equations ofstate (notably through piecewise polytropic equations of state). Using thesequasiequilibrium sequences we compute the binary's scalar charge and bindingenergy versus orbital angular frequency. We find that the absolute value of thebinding energy is smaller than in general relativity (GR), differing at most by~14% at high frequencies for the cases considered. We use the newly computedbinding energy and the balance equation to estimate the number ofgravitational-wave (GW) cycles during the adiabatic, quasicircular inspiralstage up to the end of the sequence, which is the last stable orbit or themass-shedding point, depending on which comes first. We find that, depending onthe ST parameters, the number of GW cycles can be substantially smaller than inGR. In particular, we obtain that when dynamical scalarization sets in around aGW frequency of ~130 Hz, the sole inclusion of the ST binding energy causes areduction of GW cycles from ~120 Hz up to the end of the sequence (~1200 Hz) of~11% with respect to the GR case. We estimate that when the ST energy flux isalso included the reduction in GW cycles becomes of ~24%. Quite interestingly,dynamical scalarization can produce a difference in the number of GW cycleswith respect to the GR point-particle case that is much larger than the effectdue to tidal interactions, which is on the order of only a few GW cycles. Theseresults further clarify and confirm recent studies that have evolved BNSseither in full numerical relativity or in post-Newtonian theory, and point outthe importance of developing accurate ST-theory waveforms for systems composedof strongly self-gravitating objects, such as BNSs.

Quasiequilibrium sequences of binary neutron stars undergoing dynamical scalarization