Common envelope evolution of eccentric binaries

Common envelope evolution (CEE) is believed to be an important stage in the of binary/multiple stellar systems. Following this stage, CE thought ejected, leaving behind a compact binary (or merger product). Although extensively studied, CEE process still little understood, and although most binaries have non-negligible eccentricity, effect initial eccentricity on has been explored. Moreover, studies assume complete circularization orbit by onset, while observationally such eccentricities are detected many post-CE binaries. Here we use smoothed particle hydro-dynamical simulations (SPH) study initially eccentric ($0\le e\le0.95$) CE-systems. We find that only partially circularize. In addition, higher leads following end inspiral phase, with as high 0.18 cases, even if peri-center located inside star (e.g. kick into orbit, rather than smooth transition). more enhanced dynamical mass-loss compared circular binaries, depends closest approach binary. show our results observed suggest typical assumptions orbits might potentially revised. expect affect delay time distributions various transients supernovae, gamma-ray bursts gravitational-wave sources up tens percents.