The depletion of the red supergiant envelope radiative zone during common envelope evolution

Abstract

We conduct one-dimensional stellar evolution simulations of red supergiant (RSG) stars that mimic common envelope evolution (CEE) and find that the inner boundary of the envelope convective zone moves into the initial envelope radiative zone. The envelope convection practically disappears only when the RSG radius decreases by about an order of magnitude or more. The implication is that one cannot split the CEE into one stage during which the companion spirals-in inside the envelope convective zone and removes it, and a second slower phase when the companion orbits the initial envelope radiative zone and a stable mass transfer takes place. At best, this might take place when the orbital separation is about several solar radii. However, by that time other processes become important. We conclude that as of yet, the commonly used alpha-formalism that is based on energy considerations is the best phenomenological formalism.

Research in Astronomy and Astrophysics, in press

References in corpus (20)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation
• One Channel to Rule Them All? Constraining the Origins of Binary Black Holes using Multiple Formation Pathways
• The impact of companions on stellar evolution
• Common envelope ejection in massive binary stars - Implications for the progenitors of GW150914 and GW151226
• Recombination energy in double white dwarf formation
• Common envelope events with low-mass giants: understanding the transition to the slow spiral-in
• A two-stage formalism for common-envelope phases of massive stars
• Disk formation and jet inclination effects in Common Envelopes
• The role of jets in exploding supernovae and in shaping their remnants
• From 3D hydrodynamic simulations of common-envelope interaction to gravitational-wave mergers
• Common-envelope Dynamics of a Stellar-mass Black Hole: General Relativistic Simulations
• SCATTER: A New Common Envelope Formalism
• Progenitors of low-mass binary black-hole mergers in the isolated binary evolution scenario
• Revisiting Common Envelope Evolution -- A New Semi-Analytic Model for N-body and Population Synthesis Codes
• Formation and Destiny of White Dwarf and Be Star Binaries
• Mergers of neutron stars and black holes with cores of giant stars: a population synthesis study
• Jets from main sequence and white dwarf companions during common envelope evolution
• Hot subdwarf B stars with neutron star components II: Binary population synthesis
• Formation of the First Two Black Hole-Neutron Star Mergers (GW200115 and GW200105) from Isolated Binary Evolution