Speaker
Description
Common-envelope evolution is arguably the most crucial major process in binary stars evolution, but also the least-well-constrained and more generally one of the most important unsolved challenge in stellar evolution.
Great efforts and progress have been made to confront numerical simulations outcomes to observational constraints over the last few decades. However, because of the wide range of temporal and spatial scales that need to be resolved and the associated high numerical cost, hydrodynamic simulations are often halted soon after the initial rapid in-spiral phase.
In this work, we perform the first 3D-hydrodynamic simulations focusing on the post-dynamical phase by means of an original setup mimicking the preceding rapid in-spiral. We use the Athena++ code to solve the hydrodynamics equations in spherical coordinates, exploiting its block-based adaptive mesh refinement design.
We present our numerical setup and our results regarding the secular binary separation evolution, the short-term variability of mass and angular momentum accretion onto the binary, and the (turbulent) transport of angular momentum within the shared envelope.
