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A binary neutron star merger has been observed in a multi-messenger detectionof gravitational wave (GW) and electromagnetic (EM) radiation. Binary neutronstars that merge within a Hubble time, as well as many other compact binaries,are expected to form via common envelope evolution. Yet five decades ofresearch on common envelope evolution have not yet resulted in a satisfactoryunderstanding of the multi-spatial multi-timescale evolution for the systemsthat lead to compact binaries. In this paper, we report on the first successfulsimulations of common envelope ejection leading to binary neutron starformation in 3D hydrodynamics. We simulate the dynamical inspiral phase of theinteraction between a 12$M_\odot$ red supergiant and a 1.4$M_\odot$ neutronstar for different initial separations and initial conditions. For all of oursimulations, we find complete envelope ejection and final orbital separationsof $a_{\rm f} \approx 1.3$-$5.1 R_\odot$ depending on the simulation andcriterion, leading to binary neutron stars that can merge within a Hubble time.We find $\alpha_{\rm CE}$-equivalent efficiencies of $\approx 0.1$-$2.7$depending on the simulation and criterion, but this may be specific for theseextended progenitors. We fully resolve the core of the star to $\lesssim 0.005R_\odot$ and our 3D hydrodynamics simulations are informed by an adjusted 1Danalytic energy formalism and a 2D kinematics study in order to overcome theprohibitive computational cost of simulating these systems. The framework wedevelop in this paper can be used to simulate a wide variety of interactionsbetween stars, from stellar mergers to common envelope episodes leading to GWsources.

Successful Common Envelope Ejection and Binary Neutron Star Formation in 3D Hydrodynamics