tokens: spiral-wave wind is here defined as the ejecta computed with the Bernoulli criterion discussed in Section 2.4 , and computed at times after which the dynamical ejecta have saturated. Table 4 Summary Table of the Spiral-wave Wind Properties of Long-lived Remnants Note. The columns contain the following information, starting from the left. Equation of state, mass ratio, available resolutions, inclusion of subgrid turbulence, time of the simulation end, mass of the spiral-wave wind, mass-loss rate via spiral-wave wind, mass-averaged electron fraction, terminal velocity, and finally rms angle for spiral-wave wind. For these four quantities we give the mean value among the resolutions and 1 σ deviations. For binaries for which only one resolution is present, the error is assumed to be 20% of the value. Figure 9 shows the total unbound mass of the wind as a function of time. The wind is monitored after the mass flux of the dynamical ejecta (computed according to the geodesic criterion) has saturated. Mass outflows due to the spiral-wave wind continue throughout the duration of the simulations with no indication of saturation. Indeed, while injection of mass and angular momentum from the high-density core of the remnant into the disk decreases with time as the system becomes more stationary, the mass ejection is expected to continue for as long as the spiral waves persist. Because the m = 1 modes are not efficiently damped (Paschalidis et al. 2015 ; Radice et al. 2016a ; Lehner et al. 2016b ; East et al. 2016a ), the ejection can in principle continue for the timescales that the system needs to reach equilibrium or to collapse to a BH (Section 3 ). Figure 9. Cumulative mass of the spiral-wave wind from long-lived remnants. The wind persists on timescales of ms with mass fluxes ∼0.33–1.23 M ⊙ s –1 . The largest wind masses are obtained for asymmetric binaries such as BLh q = 1.67 and LS220 q = 1.4, which in about ∼50 ms unbind ∼0.02 M ⊙ at a rate of ∼0.5 M ⊙ s –1 . We find that models with softer EOS achieve higher mass flux at lower mass ratios, i.e ., the mass flux of BLh* q = 1.66 is achieved by LS220* with q = 1.22. This might be attributed to softer EOS models having a stronger m = 1 mode in the remnant (see Section 7 ). However, if these remnants collapse, the spiral-wave mechanism shuts down and the outflow terminates. Thus the total mass ejected via spiral-wave wind depends directly on the lifetime of the remnant in addition to the binary parameters, EOS, and mass ratio. Thermal effects play an important role in determining the outflow properties, because high thermal pressures result in more extended disks with material that is easier to unbind. The highest temperatures in our simulations are found for the BLh EOS. On longer timescales than those simulated, the spiral-wave wind from the remnants with stiffer EOS might be larger, also in relation to the larger disk masses (Section 3 ). Overall, the spiral-wave wind from the long-lived remnant
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