Electromagnetic transients and r-process nucleosynthesis from the disk wind outflows of neutron star merger remnants

The remnant accretion disk formed in binaries that involve neutron stars and/or black holes is a source of non-relativistic ejecta. The outflow is launched on a viscous and/or thermal timescale, and can provide an amount of material comparable to that in the dynamical ejecta. I will present work aimed at characterizing the properties of these winds through two-dimensional, time-dependent hydrodynamic simulations that include the relevant physics needed to follow the ejecta composition. In particular, I will focus on the effect of the spin of a promptly-formed black hole remnant on the wind, and on the interaction of the disk wind with the dynamical ejecta. I will discuss the implications of these results for the optical/IR signal from these events and for the origin of r-process elements in the Galaxy.