Circumbinary Accretion: From Binary Stars to Massive Binary Black Holes

2022/10/31 by Dong Lai, Lai, Dong, Diego J. Muñoz +1 · 12 citations
Computer Science · Engineering · Physics and Astronomy · #Astrophysics and Star Formation Studies #Chemical and Environmental Engineering Research #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #Phase Equilibria and Thermodynamics #Solar and Stellar Astrophysics (astro-ph.SR)

paper · pdf · doi:10.48550/arxiv.2211.00028

openalex publication_date 2022/10/31 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

We review recent works on the dynamics of circumbinary accretion, including time variability, angular momentum transfer between the disk and the binary, and the secular evolution of accreting binaries. These dynamics can impact stellar binary formation/evolution, circumbinary planet formation/migration, and the evolution of (super)massive black-hole binaries. We discuss the dynamics and evolution of inclined/warped circumbinary disks and connect with recent observations of protoplanetary disks. A special kind of circumbinary accretion involves binaries embedded in "big" disks, which may contribute to the mergers of stellar-mass black holes in AGN disks. Highlights include: \bullet Circumbinary accretion is highly variable, being modulated at P_{\rm b} (the binary period) or ∼ 5P_{\rm p}, depending on the binary eccentricity e_{\rm b} and mass ratio q_{\rm b}. \bullet The inner region of the circumbinary disk can develop coherent eccentric structure, which may modulate the accretion and affect the physical processes (e.g. planet migration) taking place in the disk. \bullet Over long timescales, circumbinary accretion steers binaries toward equal masses, and it does not always lead to binary orbital decay, as is commonly assumed. The secular orbital evolution depends on the binary parameters (e_{\rm b} and q_{\rm b}), and on the thermodynamic properties of the accreting gas. \bullet A misaligned disk around a low-eccentricity binary tends to evolve toward coplanarity due to viscous dissipation. But when e_{\rm b} is significant, the disk can evolve toward "polar alignment", with the disk plane perpendicular to the binary plane.

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Related

• The Evolution of Accreting Binaries: from Brown Dwarfs to Supermassive Black Holes
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• On the orbital evolution of binaries with circumbinary discs
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• Circumbinary Disks: Accretion and Torque as a Function of Mass Ratio and\n Disk Viscosity