Common envelopes in massive stars III. The obstructive role of radiation transport in envelope ejection

Abstract

We present 3D radiation hydrodynamics simulations of common-envelope (CE) evolution involving a 12 solar mass red supergiant donor and a 3 solar mass companion. Existing 3D simulations are predominantly adiabatic, focusing strongly on low-mass donors on the red giant and asymptotic giant branches. However, the adiabatic assumption breaks down once the perturbed CE material becomes optically thin or when entering a longer-timescale evolutionary phase after the dynamical plunge-in. This is especially important for high-mass red supergiant donors, which have short thermal timescales, adding significant uncertainty to our understanding of how massive binary stars evolve into gravitational-wave sources, X-ray binaries, stripped-envelope supernovae, and more. We compare our radiation hydrodynamics simulations with an adiabatic simulation from Paper I that is otherwise identical, finding that radiative diffusion strongly inhibits CE ejection. The fraction of ejected mass is roughly half that of the adiabatic case without accounting for recombination energy release. Almost no material is ejected during the dynamical plunge-in, and longer-timescale ejection during the slow spiral-in is suppressed. However, the orbital separation reached at the end of the dynamical plunge-in does not differ significantly. The large amount of remaining bound mass tentatively supports the emerging view that the dynamical plunge-in is followed by a non-adiabatic phase, during which a substantial fraction of the envelope is ejected and the binary orbit may continue to evolve.

Replaced with accepted version

References in corpus (34)

• Smoothed Particle Hydrodynamics and Magnetohydrodynamics
• Modelling discontinuities and Kelvin-Helmholtz instabilities in SPH
• The Complete Evolution of a Neutron-Star Binary through a Common Envelope Phase Using 1D Hydrodynamic Simulations
• Orbital Evolution of Equal-mass Eccentric Binaries due to a Gas Disk: Eccentric Inspirals and Circular Outspirals
• Recombination energy in double white dwarf formation
• Orbital Evolution of Binaries in Circumbinary Disks
• Episodic mass ejections from common-envelope objects
• Common envelopes in massive stars: Towards the role of radiation pressure and recombination energy in ejecting red supergiant envelopes
• An Implicit Finite Volume Scheme to Solve the Time Dependent Radiation Transport Equation Based on Discrete Ordinates
• Constructing stable 3D hydrodynamical models of giant stars
• Common-envelope evolution with an asymptotic giant branch star
• Preferential Accretion and Circumbinary Disk Precession in Eccentric Binary Systems
• Energy transport by convection in the common envelope evolution
• A two-stage formalism for common-envelope phases of massive stars
• Common Envelope Evolution on a Moving Mesh
• The impact of recombination energy on simulations of the common envelope binary interaction
• Bipolar Planetary Nebulae from Outflow Collimation by Common Envelope Evolution
• Bipolar planetary nebulae from common envelope evolution of binary stars
• Long-term Evolution of Binary Orbits Induced by Circumbinary Disks
• Combining radiative transfer and diffuse interstellar medium physics to model star formation
• Binary Central Stars of Planetary Nebulae Identified With Kepler/K2
• From 3D hydrodynamic simulations of common-envelope interaction to gravitational-wave mergers
• Common envelopes in massive stars II: The distinct roles of hydrogen and helium recombination
• Convection and Spin-Up During Common Envelope Evolution: The Formation of Short-Period Double White Dwarfs
• Circumbinary discs for stellar population models
• Evolution and final fate of massive post-common-envelope binaries
• Post-dynamical inspiral phase of common envelope evolution: Binary orbit evolution and angular momentum transport
• From spherical stars to disk-like structures: 3D common-envelope evolution of massive binaries beyond inspiral
• Stable anisotropic heat conduction in smoothed particle hydrodynamics
• Dust formation in common envelope binary interactions -- II: 3D simulations with self-consistent dust formation
• Simulating a stellar contact binary merger -- I. Stellar models
• Magnetically driven outflows in 3D common-envelope evolution of massive stars
• Journey to the center of the common envelope evolution. Inner dynamics of the post-dynamical inspiral
• The Energy Sharing Timescale in an Analytic Framework for Common Envelope Hydrodynamics

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