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We present a systematic numerical-relativity study of the dynamical ejecta,winds and nucleosynthesis in neutron star merger remnants. Binaries with thechirp mass compatible with GW170817, different mass ratios, and fivemicrophysical equations of state (EOS) are simulated with an approximateneutrino transport and a subgrid model for magnetohydrodynamics turbulence upto 100 milliseconds postmerger. Spiral density waves propagating from theneutron star remnant to the disk trigger a wind with mass flux${\sim}0.1{-}0.5\,{\rm M_\odot/s}$ persisting for the entire simulation as longas the remnant does not collapse to black hole. This wind has average electronfraction $\gtrsim 0.3$ and average velocity ${\sim}0.1-0.17\,$c and thus is asite for the production of weak $r$-process elements (mass number $A<195$).Disks around long-lived remnants have masses ${\sim}0.1{-}0.2\,{\rm M_\odot}$,temperatures peaking at $\lesssim10\,$MeV near the inner edge, and acharacteristic double-peak distribution in entropy resulting from shockspropagating through the disk. The dynamical and spiral-wave ejecta computed inour targeted simulations are not compatible with those inferred from AT2017gfousing two-components kilonova models. Rather, they indicate thatmulti-component kilonova models including disk winds are necessary to interpretAT2017gfo. The nucleosynthesis in the combined dynamical ejecta and spiral-wavewind in the comparable-mass long-lived mergers robustly accounts for all the$r$-process peaks, from mass number ${\sim}75$ to actinides in terms of solarabundances. Total abundandes are weakly dependent on the EOS, while the massratio affect the production of first peak elements.

Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-Term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis