Dust formation in common envelope binary interactions -- II: 3D simulations with self-consistent dust formation

Abstract

We performed numerical simulations of the common envelope (CE) interaction between thermally-pulsing asymptotic giant branch (AGB) stars of 1.7~\Msun and 3.7~\Msun, respectively, and a 0.6~\Msun compact companion. We use tabulated equations of state to take into account recombination energy. For the first time, formation and growth of dust is calculated explicitly, using a carbon dust nucleation network with a C/O abundance ratio of 2.5 (by number). The first dust grains appear within $\sim$1--3~yrs after the onset of the CE, forming an optically thick shell at $\sim$10--20~au, growing in thickness and radius to values of $\sim$400--500~au over $\sim$40~yrs, with temperatures around 400~K. Most dust is formed in unbound material, having little effect on mass ejection or orbital evolution. By the end of the simulations, the total dust yield is $\sim 8.4\times 10^{-3}$~\Msun and $\sim 2.2\times 10^{-2}$~\Msun for the CE with a 1.7~\Msun and a 3.7~\Msun AGB star, respectively, corresponding to a nucleation efficiency close to 100\%, if no dust destruction mechanism is considered. Despite comparable dust yields to single AGB stars, \textit{in CE ejections the dust forms a thousand times faster, over tens of years as opposed to tens of thousands of years}. This rapid dust formation may account for the shift in the infrared of the spectral energy distribution of some optical transients known as luminous red novae. Simulated dusty CEs support the idea that extreme carbon stars and "water fountains" may be objects observed after a CE event.

18 pages, 17 figures, 2 tables

References in corpus (35)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars
• Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
• Common Envelope Evolution: Where we stand and how we can move forward
• V1309 Scorpii: merger of a contact binary
• Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
• Low-Mass Binary Induced Outflows from Asymptotic Giant Branch Stars
• The impact of companions on stellar evolution
• Common Envelope ejection for a Luminous Red Nova in M101
• Dust from AGBs: relevant factors and modelling uncertainties
• SPIRITS: Uncovering Unusual Infrared Transients With Spitzer
• On the role of recombination in common-envelope ejections
• Discovery of a new photometric sub-class of faint and fast classical novae
• Extending Common Envelope Simulations from Roche Lobe Overflow to the Nebular Phase
• Luminosities and mass-loss rates of Local Group AGB stars and Red Supergiants
• Common envelopes in massive stars: Towards the role of radiation pressure and recombination energy in ejecting red supergiant envelopes
• Efficient common-envelope ejection through dust-driven winds
• Gas and dust from solar metallicity AGB stars
• Constraints on Common Envelope Magnetic Fields from Observations of Jets in Planetary Nebulae
• Discovery of Extreme Carbon Stars in the Large Magellanic Cloud
• The Dusty Aftermath of the V1309 Sco Binary Merger
• The effect of binding energy and resolution in simulations of the common envelope binary interaction
• The impact of recombination energy on simulations of the common envelope binary interaction
• Light Curve Model for Luminous Red Novae and Inferences about the Ejecta of Stellar Mergers
• Formulation of Non-steady-state Dust Formation Process in Astrophysical Environments
• Dust Formation in the Ejecta of Common Envelope Systems
• Properties of the post in-spiral common envelope ejecta II: dust formation
• A 3D radiation-hydrodynamic AGB binary model
• Properties of the post in-spiral common envelope ejecta I: dynamical and thermal evolution
• AGB winds in interacting binary stars
• Observational identification of a sample of likely recent Common-Envelope Events
• 3D simulations of AGB stellar winds -- I. Steady winds and dust formation
• Dusty, Self-obscured Transients from Stellar Coalescence
• Are extreme AGB stars post-common envelope binaries?
• Dust Formation in Common Envelope Binary Interaction -- I: 3D Simulations Using the Bowen Approximation

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