Common Envelope Evolution of Massive Stars

Abstract

The discovery via gravitational waves of binary black hole systems with total masses greater than $60M_{\odot }$ has raised interesting questions for stellar evolution theory. Among the most promising formation channels for these systems is one involving a common envelope binary containing a low metallicity, core helium burning star with mass $\sim 80-90M_{\odot }$ and a black hole with mass $\sim 30-40M_{\odot }$. For this channel to be viable, the common envelope binary must eject more than half the giant star's mass and reduce its orbital separation by as much as a factor of 80. We discuss issues faced in numerically simulating the common envelope evolution of such systems and present a 3D AMR simulation of the dynamical inspiral of a low-metallicity red supergiant with a massive black hole companion.

6 pages, 3 figures, oral contribution: IAU Symposium 346 "High Mass X-ray Binaries: illuminating the passage from massive binaries to merging compact objects", Vienna, Austria, 27-31 August 2018

References in corpus (12)

• Modules for Experiments in Stellar Astrophysics (MESA)
• GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence
• Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions
• The Interaction of Stellar Objects within a Common Envelope
• A Direct Multigrid Poisson Solver for Oct-Tree Adaptive Meshes
• Accretion in common envelope evolution
• Recombination energy in double white dwarf formation
• Three Dimensional Radiation Hydrodynamic Simulations of Massive Star Envelopes
• Accretion Disk Assembly During Common Envelope Evolution: Implications for Feedback and LIGO Binary Black Hole Formation
• On the use of hydrogen recombination energy during common envelope events
• Radiating the hydrogen recombination energy during common envelope evolution
• Energizing the last phase of common envelope removal

Cited by in corpus (13)

• Rates of Compact Object Coalescences
• Common envelopes in massive stars: Towards the role of radiation pressure and recombination energy in ejecting red supergiant envelopes
• Common-envelope evolution with an asymptotic giant branch star
• The Common Envelope Evolution Outcome -- A Case Study on Hot Subdwarf B Stars
• 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
• Octo-Tiger: A New, 3D Hydrodynamic Code for Stellar Mergers that uses HPX Parallelisation
• Convection Reconciles the Difference in Efficiencies Between Low-Mass and High-Mass Common Envelopes
• Formation and Evolution of Accreting Compact Objects
• Two-Dimensional Radiation-Hydrodynamic Simulations of Luminous Red Novae
• Stellar response after stripping as a model for common-envelope outcomes
• Light Curve Models of Convective Common Envelopes
• Inferring binary black holes stellar progenitors with gravitational wave sources