The influence of equation of state on impact dynamics between Pluto-like bodies

Impacts between planetary-sized bodies can explain the origin of satellites orbiting large ($R>500$~km) trans-Neptunian objects. Their water rich composition, along with complex phase diagram water, make it important to accurately model wide range thermodynamic conditions material experiences during an impact event and in debris disk. Since differences thermodynamics may influence system dynamics, we seek evaluate how choice equation state (EOS) alters system's evolution. Specifically, compare two EOSs that are constructed by different approaches: either a simplified analytic description (Tillotson), or interpolation tabulated data (Sesame). Approximately $50$ pairs Smoothed Particle Hydrodynamics simulations were performed, similar initial but EOSs, parameter space which Pluto-Charon binary is thought form (slow impacts Pluto-size, bodies). Generally, show outcomes (e.g., circumplanetary disk) consistent EOSs. Some arise, importantly production satellitesimals (large intact clumps) post-impact When utilizing EOS, emergence highly certain, while when using EOS less common. This because for typical densities energies experienced these impacts, predicts very low pressure values, leading particles artificially aggregating tensile instability.