Post-dynamical inspiral phase of common envelope evolution: Binary orbit evolution and angular momentum transport

TL;DR

This study uses 3D hydrodynamical simulations to explore the complex angular momentum transport and orbital evolution of binary systems after the dynamical plunge phase of common envelope evolution, revealing sustained orbital decay and envelope dynamics.

Contribution

It provides the first systematic multidimensional simulation analysis of the post-dynamical phase, highlighting the roles of advection, turbulence, and gravitational torques in angular momentum transport.

Findings

Angular momentum transport is dominated by advection and Reynolds stresses.

Envelope shows disk-like structures with inward and outward angular momentum flow.

Orbital decay timescale stabilizes around 10^3 to 10^4 binary orbits with accretion, longer without.

Abstract

After the companion dynamically plunges through the primary's envelope, the two cores remain surrounded by a common envelope and the decrease of the orbital period $P_\text{orb}$ stalls. The subsequent evolution has never been systematically explored with multidimensional simulations. For this study, we performed 3D hydrodynamical simulations of an envelope evolving under the influence of a central binary star using an adaptively refined spherical grid. We followed the evolution over hundreds of orbits of the central binary to characterize the transport of angular momentum by advection, gravitational torques, turbulence, and viscosity. We find that local advective torques from the mean flow and Reynolds stresses associated with the turbulent flow dominate the angular momentum transport, which occurs outward in a disk-like structure about the orbital plane and inward along the polar axis. Turbulent transport is less efficient, but can locally significantly damp or enhance the net angular momentum radial transport and may even reverse its direction. Short-term variability in the envelope is remarkably similar to circumbinary disks, including the formation and destruction of lump-like overdensities, which enhance mass accretion and contribute to the outward transport of eccentricity generated in the vicinity of the binary. If the accretion onto the binary is allowed, the orbital decay timescale settles to a nearly constant value $\tau_\text{b} \sim 10^3$ to $10^4\,P_\text{orb}$, while preventing accretion leads to a slowly increasing $\tau_\text{b} \sim 10^5\,P_\text{orb}$ at the end of our simulations. Our results suggest that the post-dynamical orbital contraction and envelope ejection will slowly continue while the binary is surrounded by gas and that $\tau_\text{b}$ is often much shorter than the thermal timescale of the envelope.