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Short gamma-ray bursts require a rotating black hole, surrounded by amagnetized relativistic accretion disk, such as the one formed by coalescingbinary neutron stars or neutron star - black hole systems. The accretion onto aKerr black hole is the mechanism of launching a baryon-free relativistic jet.An additional uncollimated outflow, consisting of sub-relativistic neutron-richmaterial which becomes unbound by thermal, magnetic and viscous forces, isresponsible for blue and red kilonova. We explore the formation, compositionand geometry of the secondary outflow by means of simulating accretion diskswith relativistic magneto-hydrodynamics and employing realistic nuclearequation of state. We calculate the nucleosynthetic r-process yields bysampling the outflow with a dense set of tracer particles. Nuclear heating fromthe residual r-process radioactivities in the freshly synthesized nuclei isexpected to power a red kilonova, contributing independently from the dynamicalejecta component, launched at the time of merger, and neutron-poor broad polaroutflow, launched from the surface of the hypermassive neutron star by neutrinowind. Our simulations show that both magnetisation of the disk and high blackhole spin are able to launch fast wind outflows ($v/c\sim 0.11-0.23$) with abroad range of electron fraction $Y_{\rm e}\sim 0.1-0.4$, and help explain themultiple components observed in the kilonova lightcurves. The total mass lossfrom the post-merger disk via unbound outflows is between 2\% and 17\% of theinitial disk mass.

The r-process nucleosynthesis in the outflows from short GRB accretion disks