The Hydrodynamic Evolution of Binary Black Holes Embedded within the Vertically Stratified Disks of Active Galactic Nuclei

Kaaz, Nicholas; Schröder, S.; Andrews, Jeff J.; Antoni, Andrea; Ramírez-Ruiz, E.

doi:10.3847/1538-4357/aca967

Cited by 16 publications

(9 citation statements)

References 120 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…When this happens, the embedded BHs can migrate, accrete at super-Eddington rates, and potentially produce electromagnetic transients. The accretion geometry of the sBH-AGN binary depends mainly on the mass ratio of the system and the AGN disk scale height (Kaaz et al 2023). If the mass ratio is large, then the system resembles more traditional circumbinary disks, where the sBH can impact the structure of the host disk (Baruteau et al 2011;Li et al 2021).…”

Section: Disks Of Active Galactic Nucleimentioning

confidence: 99%

“…A black hole (BH) traversing through a gaseous medium is common in a wide variety of astrophysical scenarios, including common envelope evolution (MacLeod & Ramirez-Ruiz 2015;MacLeod et al 2017;Murguia-Berthier et al 2017;Everson et al 2020), wind accretion in binary systems (El Mellah & Casse 2015;El Mellah et al 2018), and the passage of stellarmass BHs through the disks of active galactic nuclei (Stone et al 2017;Kaaz et al 2023). As the BH travels through the medium, it will accrete mass and potentially produce energetic outflows that alter its environment.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Jet Formation in 3D GRMHD Simulations of Bondi–Hoyle–Lyttleton Accretion

Kaaz

Murguia-Berthier²,

Chatterjee

et al. 2023

ApJ

Self Cite

View full text Add to dashboard Cite

A black hole (BH) traveling through a uniform, gaseous medium is described by Bondi–Hoyle–Lyttleton (BHL) accretion. If the medium is magnetized, then the black hole can produce relativistic outflows. We performed the first 3D, general-relativistic magnetohydrodynamic simulations of BHL accretion onto rapidly rotating black holes using the H-AMR code, where we mainly varied the strength of a background magnetic field that threads the medium. We found that the ensuing accretion continuously drags the magnetic flux to the BH, which accumulates near the event horizon until it becomes dynamically important. Depending on the strength of the background magnetic field, the BHs can sometimes launch relativistic jets with high enough power to drill out of the inner accretion flow, become bent by the headwind, and escape to large distances. For stronger background magnetic fields, the jets are continuously powered, while at weaker field strengths they are intermittent, turning on and off depending on the fluctuating gas and magnetic flux distributions near the event horizon. We find that our jets reach extremely high efficiencies of ∼100%–300%, even in the absence of an accretion disk. We also calculated the drag forces exerted by the gas onto to the BH and found that the presence of magnetic fields causes the drag forces to be much less efficient than in unmagnetized BHL accretion. They can even sometimes become negative, accelerating the BH rather than slowing it down. Our results extend classical BHL accretion to rotating BHs moving through magnetized media, and demonstrate that accretion and drag are significantly altered in this environment.

show abstract

Section: Disks Of Active Galactic Nucleimentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Jet Formation in 3D GRMHD Simulations of Bondi–Hoyle–Lyttleton Accretion

Kaaz

Murguia-Berthier²,

Chatterjee

et al. 2023

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…The jet-cocoon evolution can also generate mechanical feedback to suppress the accretion of BH in the AGN disk (Kaaz et al 2023;Tagawa et al 2022). Assuredly, L MAD > L w may cause jet other than wind dominants the feedback.…”

Section: Jet Effect and Outflow Em Radiationmentioning

confidence: 99%

“…The CO mass capturing rate is generally hyper-Eddington, which may even exceed the mass inflow rate of the AGN disk. Previous works have artificially set upper limits for the accretion rate onto CO at the Eddington rate with various radiative efficiencies, or at the AGN disk mass inflow rate, or directly at a certain fraction of CO mass capturing rate (e.g., Tagawa et al 2020a;McKernan et al 2020b;Wang et al 2021a;Kimura et al 2021b;Kaaz et al 2023), but none has yet connected the rate to the actual accretion processes of CO. Hyper-Eddington accretion is predicted both theoretically and by numerical simulations to be accompanied by a powerful outflow of mass and energy in the form of circum-CO disk wind and collimated jet (e.g., Blandford & Begelman 1999;Ohsuga et al 2005;Begelman 2012;Gu 2012;Jiang et al 2014;Yang et al 2014;Gu 2015;Hashizume et al 2015;Saḑowski & Narayan 2016;Kitaki et al 2018;Hu et al 2022), which reduces the mass rate eventually accreted onto COs (Pan & Yang 2021b), and conversely interacts with surroundings, acting as feedback. Several recent works have investigated the feedback of CO hyper-Eddington accretion on the AGN disk environment (Wang et al 2021a;Kimura et al 2021b;Tagawa et al 2022), where Wang et al (2021a) and Kimura et al (2021b) did not concretely discuss the properties of the disk wind, while Tagawa et al (2022) mainly focused on the jetcocoon feedback from high-spin stellar-mass BHs, which may not be practical for low-spin BHs and NSs.…”

Section: Introductionmentioning

confidence: 99%

The Role of Outflow Feedback on Accretion of Compact Objects in Accretion Disk of Active Galactic Nuclei

Chen

Ren

Dai

2023

ApJ

View full text Add to dashboard Cite

Compact objects (COs) can exist and evolve in an active galactic nuclei (AGN) disk, triggering a series of attractive CO-related multimessenger events around a supermassive black hole. To better understand the nature of an embedded CO and its surroundings and to investigate CO-related events more accurately, in this paper, we study the specific accretion process of a CO in an AGN disk and explore the role of outflow feedback. We show that the asymptotically isotropic outflow generated from the CO hyper-Eddington accretion would truncate the circum-CO disk and push out its surrounding gas, resulting in recurrent formation and refilling of an outflow cavity to intermittently stop the accretion. Applying this universal cyclic process to black holes (BHs) and neutron stars (NSs), we find that, even if it is above the Eddington rate, the mass rate accreted onto a BH is dramatically reduced compared with the initial gas captured rate and thus consumes little mass of the AGN disk; outflow feedback on an NS is generally similar, but possesses complexities on the existence of a stellar magnetic field and hard surface. We demonstrate that although outflow feedback itself may be unobservable, it remarkably alters the CO evolution via reducing its mass growth rate, and the AGN disk can survive from the otherwise drastic CO accretion overlooking outflow. In addition, we discuss the potential influence of an underdense cavity on CO-related events, which embodies the significant role of outflow feedback as well.

show abstract

“…Additionally, star-BH binaries in an AGN disk can become tightly bound due to external torques exerted by the dynamical friction of the AGN disk gas. Hydrodynamical simulations have shown that a circumbinary disk tends to shrink the orbit of the binary within an AGN disk (Li et al 2021;Kaaz et al 2021;Li & Lai 2022) and drive it to low eccentricity, either e → 0 or e → 0.45, depending on the initial value (Muñoz et al 2019;D'Orazio & Duffell 2021;Zrake et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Tidal Peeling Events: low-eccentricity tidal disruption of a star by a stellar-mass black hole

Xin¹,

Haiman²,

Perna³

et al. 2023

Preprint

View full text Add to dashboard Cite

Close encounters between stellar-mass black holes (BHs) and stars occur frequently in dense star clusters and in the disks of active galactic nuclei (AGNs). Recent studies have shown that in highly eccentric close encounters, the star can be tidally disrupted by the BH (micro-tidal disruption event, or micro-TDE), resulting in rapid mass accretion and possibly bright electromagnetic signatures. Here we consider a scenario in which the star might approach the stellar-mass BH in a gradual, nearly circular inspiral, under the influence of dynamical friction on a circum-binary gas disk or three-body interactions in a star cluster. We perform hydro-dynamical simulations of this scenario using the smoothed particle hydrodynamics code PHANTOM. We find that the mass of the star is slowly stripped away by the BH. We call this gradual tidal disruption a "tidal-peeling event", or a TPE. Depending on the initial distance and eccentricity of the encounter, TPEs might exhibit significant accretion rates and orbital evolution distinct from those of a typical (eccentric) micro-TDE.

show abstract

The Hydrodynamic Evolution of Binary Black Holes Embedded within the Vertically Stratified Disks of Active Galactic Nuclei

Cited by 16 publications

References 120 publications

Jet Formation in 3D GRMHD Simulations of Bondi–Hoyle–Lyttleton Accretion

Jet Formation in 3D GRMHD Simulations of Bondi–Hoyle–Lyttleton Accretion

The Role of Outflow Feedback on Accretion of Compact Objects in Accretion Disk of Active Galactic Nuclei

Tidal Peeling Events: low-eccentricity tidal disruption of a star by a stellar-mass black hole

Contact Info

Product

Resources

About