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The observation of a radioactively-powered kilonova associated with the firstbinary neutron star (BNS) merger detected in gravitational waves proved thatthese events are ideal sites for the production of heavy r-process elements.However, the physical origin of the ejected material responsible for the early("blue") and late ("red") components of this kilonova is still debated. Here,we investigate the possibility that the early/blue kilonova originated from themagnetically driven baryon wind launched after merger by the metastable neutronstar remnant. Exploiting a magnetized BNS merger simulation with over 250 ms ofpost-merger evolution, we can follow for the first time the full mass ejectionprocess up to its final decline. We find that the baryon wind carries$\simeq\!0.010\!-\!0.028\,M_\odot$ of unbound material, proving that the highmass estimated for the blue kilonova can be achieved. We also find expansionvelocities of up to $\sim\!0.2\,c$, consistent with the lower end of theobservational estimates, and we discuss possible effects neglected here thatcould further increase the final ejecta velocity. Overall, our results showthat the magnetically driven baryon wind represents a viable channel to explainthe blue kilonova.

Magnetically driven baryon winds from binary neutron star merger remnants and the blue kilonova of August 2017