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Following the detection of GW170817 and the accompanying kilonova AT2017gfo,it has become crucial to model and understand the various channels throughwhich mass is ejected in neutron-star binary mergers. We discuss the impactthat high stellar spins prior to merger have on the ejection of mass focussing,in particular, on the dynamically ejected mass by performinggeneral-relativistic magnetohydrodynamic simulations employingfinite-temperature equations of state and neutrino-cooling effects. Using eightdifferent models with dimensionless spins ranging from $\chi\simeq-0.14$ to$\chi\simeq0.29$ we discuss how the presence of different spins affects theangular distribution and composition of the ejected matter. Most importantly,we find that the dynamical component of the ejected mass can be stronglysuppressed in the case of high spins aligned with the orbital angular momentum.In this case, in fact, the merger remnant has an excess angular momentumyielding a more extended and "colder" object, with reduced ability to shed massdynamically. We discuss how this result impacts the analysis of the recentmerger event GW170817 and its kilonova afterglow.

Impact of high spins on the ejection of mass in GW170817