Preferential accretion onto eccentric and unequal binary black holes
Abstract
Supermassive binary black holes (SMBBHs) are expected to be surrounded by circumbinary disks (CBDs) which affect the binary through gravitational forces and accretion. It has been reported that the binary can experience ``preferential accretion'' where one black hole (BH) out-accretes the other for hundreds of orbits, but this asymmetry has yet to be fully described or understood. In this work, we utilize a suite of 80 SMBBH hydrodynamical simulations with varying mass ratios (qb) and eccentricity (eb) in order to robustly delineate the behavior of preferential accretion, determine its relationship to the structure of the CBD, and study its observational consequences. We characterize the accretion-rate ratio λ(t) ≡ Ṁ2(t)/Ṁ1(t) and the mass-ratio rate of change q̇b ≡ d/dt(M2/M1) across the suite. We confirm that the secondary tends to out-accrete the primary (λ≥ 1), and find this preference to be strongest for low-eb, low-qb binaries and increasingly time-variable toward high eb. We also find that (i) the time-variability of λ tracks the precession of the CBD, (ii) there can be sub- and super-Eddington accretion in a single binary, and (iii) the gas-driven approach toward equal mass becomes particularly slow for highly eccentric, high qb binaries, suggesting that some binaries may not reach qb=1 within the 30 Myr lifetime of a quasar and therefore allowing LISA to constrain the accretion history of SMBBHs. Our findings also suggest that periodically flickering jets are a potential observable signature of many binaries.
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BibTeX
@misc{delaurentiis2026preferential,
title = {{Preferential accretion onto eccentric and unequal binary black holes}},
author = {Stanislav DeLaurentiis and Zoltán Haiman and Magdalena Siwek},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.04491},
eprint = {2609.04491},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.04491},
}
RIS
TY - UNPB
TI - Preferential accretion onto eccentric and unequal binary black holes
AU - Stanislav DeLaurentiis
AU - Zoltán Haiman
AU - Magdalena Siwek
PY - 2026
DA - 2026/09/03
PB - arXiv
DO - 10.48550/arxiv.2609.04491
UR - https://arxiv.org/abs/2609.04491
AB - Supermassive binary black holes (SMBBHs) are expected to be surrounded by circumbinary disks (CBDs) which affect the binary through gravitational forces and accretion. It has been reported that the binary can experience ``preferential accretion'' where one black hole (BH) out-accretes the other for hundreds of orbits, but this asymmetry has yet to be fully described or understood. In this work, we utilize a suite of 80 SMBBH hydrodynamical simulations with varying mass ratios (q_b) and eccentricity (e_b) in order to robustly delineate the behavior of preferential accretion, determine its relationship to the structure of the CBD, and study its observational consequences. We characterize the accretion-rate ratio λ(t) ≡ Ṁ_2(t)/Ṁ_1(t) and the mass-ratio rate of change q̇_b ≡ d/dt(M_2/M_1) across the suite. We confirm that the secondary tends to out-accrete the primary (λ≥ 1), and find this preference to be strongest for low-e_b, low-q_b binaries and increasingly time-variable toward high e_b. We also find that (i) the time-variability of λ tracks the precession of the CBD, (ii) there can be sub- and super-Eddington accretion in a single binary, and (iii) the gas-driven approach toward equal mass becomes particularly slow for highly eccentric, high q_b binaries, suggesting that some binaries may not reach q_b=1 within the 30 Myr lifetime of a quasar and therefore allowing LISA to constrain the accretion history of SMBBHs. Our findings also suggest that periodically flickering jets are a potential observable signature of many binaries.
ER -