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Short Gamma-Ray Bursts (GRBs) are known to be associated with binary neutronstar (NSNS) or black hole-neutron star (BHNS) mergers. The detection ofgravitational wave and its associated electromagnetic counterparts GW/GRB170817A has shown that interactions between relativistic jets and mildlyrelativistic ejecta influence observed radiation. Previous studies simulated auniform jet propagating through a homologously expanding wind, however, jetsand disk outflows are launched together during accretion, making theinteraction more complex. We investigate how the disk wind impacts jetpropagation at distances $r\sim 10^8\,-\,10^{11}~$cm. We are usingtwo-dimensional special relativistic hydrodynamical simulations. As initialconditions, we remap the outflows from general relativisticmagnetohydrodynamical simulations of BH accretion disks that representpost-merger NSNS or BHNS remnants. We account for wind stratification andr-process nucleosynthesis, which alter the pressure profile from that of anideal gas in the initial conditions. We found that a) self-consistent windpressure leads to significant changes in the jet collimation and cocoonexpansion; b) the angular structure of thermal and kinetic energy components inthe jets, cocoons, and winds differ with respect to simple homologous models;c) the temporal evolution of the structure reveals conversion of thermal tokinetic energy being different for each component in the system (jet, cocoon,and wind); d) dynamical ejecta alters the interaction between jets and diskwinds. Our results show that the jet and cocoon structure is shaped by theaccretion disk wind that alters the effect of dynamical ejecta and may have animpact on the observed afterglow emission.

The impact of disk outflows on the structure of short GRB jets at large scales