Ultrarelativistic Bondi–Hoyle accretion – I. Axisymmetry

Penner, A. J.

doi:10.1093/mnras/sts176

Cited by 14 publications

(11 citation statements)

References 23 publications

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“…While magnetized BHL accretion has been studied generally (Lee et al 2014), it is particularly intriguing if the central object is a BH,because relativistic jets may then be launched. Nonmagnetized relativistic BHL accretion has been simulated in the past (Font & Ibáñez 1998;Lora-Clavijo & Guzmán 2013;Penner 2013;Koyuncu & Dönmez 2014;Blakely & Nikiforakis 2015;Gracia-Linares & Guzmán 2015;Lora-Clavijo et al 2015;Cruz-Osorio et al 2017), as has 2D magnetized relativistic BHL accretion (Penner 2011), but (to the best of our knowledge) our work is the first to simulate 3D generalrelativistic magnetohydrodynamic (GRMHD) BHL accretion.…”

Section: Introductionmentioning

confidence: 99%

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

Kaaz

Murguia-Berthier²,

Chatterjee

et al. 2023

ApJ

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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.

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Section: Introductionmentioning

confidence: 99%

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

Kaaz

Murguia-Berthier²,

Chatterjee

et al. 2023

ApJ

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“…While magnetized BHL accretion has Corresponding author: Nicholas Kaaz nkaaz@u.northwestern.edu * NASA Einstein Fellow been studied generally (Lee et al 2014), it is particularly intriguing if the central object is a BH, because then relativistic jets may be launched. Non-magnetized relativistic BHL accretion has been simulated in the past (Font & Ibáñez 1998;Penner 2013;Lora-Clavijo & Guzmán 2013;Koyuncu & Dönmez 2014;Gracia-Linares & Guzmán 2015;Lora-Clavijo et al 2015;Blakely & Nikiforakis 2015;Cruz-Osorio et al 2017), as has 2D magnetized relativistic BHL accretion (Penner 2011), but to the best of our knowledge, our work is the first to simulate 3D general-relativistic magnetohydrodynamic (GRMHD) BHL accretion.…”

Section: Introductionmentioning

confidence: 99%

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

Kaaz¹,

Murguia-Berthier²,

Chatterjee³

et al. 2022

Preprint

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A black hole (BH) travelling 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 magnetohydrodynamics simulations of BHL accretion onto rapidly rotating black holes using the code H-AMR, where we mainly varied the strength of a background magnetic field that threads the medium. We found that the ensuing accretion continuously drags to the BH the magnetic flux, 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. While for stronger background magnetic fields the jets are continuously powered, 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, finding that the presence of magnetic fields causes drag forces to be much less efficient than in unmagnetized BHL accretion, and 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.

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“…2D and 3D numerical simulations of the accretion disk had accomplished to reveal the dynamical structure of the disk, radiation mechanism, and properties of the compact objects (Foglizzo et al 2005;Blondin 2013;MacLeod & Ramirez-Ruiz 2015;Ohsugi 2018;Xu & Stone 2019). Non-magnetized or magnetized relativistic BHL accretions around the non-rotating and rotating black holes have been simulated using either axial or spherical symmetries (Dönmez et al 2011;Penner 2011;Dönmez 2012;Penner 2012;Lora-Clavijo & Guzmán 2013;Koyuncu & Dönmez 2014;Lora-Clavijo et al 2015;Gracia-Linares & Guzmán 2015;Cruz-Osorio & Lora-Clavijo 2016).…”

Section: Introductionmentioning

confidence: 99%

Study of Asymptotic Velocity in the Bondi-Hoyle Accretion Flows in the Domain of Kerr and 4-D Einstein-Gauss-Bonnet Gravities

Dönmez¹,

Doğan²,

Şahin³

2022

Preprint

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Understanding the physical structures of the accreated matter very close to the black hole in quasars and active galactic nucleus (AGNs) is an important milestone to constrain the activities occurring in their centers. In this paper, we numerically investigate the effects of the asymptotic velocities on the physical structures of the accretion disk around the Kerr and Einstein-Gauss-Bonnet (EGB) rapidly rotating black holes. The Bondi-Hoyle accretion is considered with a falling gas towards the black hole in upstream region of the computational domain. The shock cones are naturally produced in the downstream part of the flow around both black holes. It is found that the structure of the cones and the amount of the accreated matter depend on asymptotic velocity V ∞ (Mach number) and the types of the gravities (Kerr or EGB). Increasing the Mach number of the inflowing matter in the supersonic region causes the shock opening angle and accretion rates getting smaller because of the rapidly falling gas towards the black hole. The EGB gravity leads to an increase in the shock opening angle of the shock cones while the mass accretion rates Ṁ are decreasing in EGB gravity with a Gauss-Bonnet (GB) coupling constant α. It is also confirmed that accretion rates and drag forces are significantly altered in the EGB gravity. Our numerical simulation results could be used to identify the accreation mechanism and physical properties of the accretion disk and black hole in the observed X− rays such as NGC 1313 X − 1 and 1313 X − 2 and MAXI J1803 − 298.

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Ultrarelativistic Bondi–Hoyle accretion – I. Axisymmetry

Cited by 14 publications

References 23 publications

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

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

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

Study of Asymptotic Velocity in the Bondi-Hoyle Accretion Flows in the Domain of Kerr and 4-D Einstein-Gauss-Bonnet Gravities

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