  Short Gamma-Ray Bursts (GRBs) are often associated with NSNS or BHNS mergers.
The discovery of GW/GRB 170817A has enhanced our understanding, revealing that
the interaction between relativistic jets and post-merger outflows influences
the observed radiation. However, the nature of compact binary merger event
suggests that the system can be more complex than the uniform jet interacting
with a homologously expanding wind. We consider here an improved scenario by
performing a set of two-dimensional, large scale numerical simulations, and we
investigate the interaction between short GRB jets and post-merger disk wind
outflows. We focus on two types of configurations, arising from NSNS and BHNS
mergers. The simulations consider the effects of the r-process nucleosynthesis
in the accretion disk wind on its pressure profile. The main properties of the
jet, such as its energy distribution and collimation degree, are estimated from
our simulations. We found that a) the impact of the r-process on initial wind
pressure leads to significant changes in the jet collimation and cocoon
expansion; b) the angular structure of thermal and kinetic energy components in
the jets, cocoons, and winds differ with respect to simple homologous models,
hence it would affect the predictions of GRB afterglow emission; c) the
temporal evolution of the structure reveals conversion of thermal to kinetic
energy being different for each component in the system (jet, cocoon, and
wind); d) post-merger environments influence energy structure and material
dispersion, altering the interaction between jets and disk winds. %Our study
underscores the importance of post-merger disk wind in the jet propagation,
emphasizing the need for careful parameter selection to avoid interpretation
degeneracy in the electromagnetic counterparts.
