The Jet–disk Boundary Layer in Black Hole Accretion

Wong, George N.; Du, Yufeng; Prather, Ben; Gammie, Charles F.

doi:10.3847/1538-4357/abf8b8

Cited by 26 publications

(25 citation statements)

References 49 publications

(58 reference statements)

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“…The jet in retrograde simulations rotates in the same sense as the BH, which is opposite to the direction of the disk angular momentum at large radii. The resulting boundary layer between the co-rotating jet and counter-rotating disk is unstable, and plasma is loaded onto the jet field lines in fluctuating episodic events (Wong et al 2021).…”

Section: Disk and Jet Structurementioning

confidence: 99%

Jets in Magnetically Arrested Hot Accretion Flows: Geometry, Power and Black Hole Spindown

Narayan,

Chael,

Chatterjee

et al. 2021

Preprint

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We present the results of nine simulations of radiatively-inefficient magnetically arrested disks (MADs) across different values of the black hole spin parameter a * : −0.9, −0.7, −0.5, −0.3, 0, 0.3, 0.5, 0.7, and 0.9. Each simulation was run up to t 100, 000 GM/c 3 to ensure disk inflow equilibrium out to large radii. We find that the saturated magnetic flux level, and consequently also jet power, of MAD disks depends strongly on the black hole spin, confirming the results of . Prograde disks saturate at a much higher relative magnetic flux and have more powerful jets than their retrograde counterparts. MADs with spinning black holes naturally launch jets with generalized parabolic profiles with width varying as a power of distance from the black hole. For distances up to 100GM/c 2 , the power-law index is k ≈ 0.27−0.42. There is a strong correlation between the disk-jet geometry and the dimensionless magnetic flux, resulting in prograde systems displaying thinner equatorial accretion flows near the black hole and wider jets, compared to retrograde systems. Prograde and retrograde MADs also exhibit different trends in disk variability: accretion rate variability increases with increasing spin for a * > 0 and remains almost constant for a * 0, while magnetic flux variability shows the opposite trend. Jets in the MAD state remove more angular momentum from black holes than is accreted, effectively spinning down the black hole. If powerful jets from MAD systems in Nature are persistent, this loss of angular momentum will notably reduce the black hole spin over cosmic time.

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Section: Disk and Jet Structurementioning

confidence: 99%

Jets in Magnetically Arrested Hot Accretion Flows: Geometry, Power and Black Hole Spindown

Narayan,

Chael,

Chatterjee

et al. 2021

Preprint

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“…The viewing inclination is chosen so that the black hole spin vector is always oriented away from the viewer at an angle of 17 • from the screen normal, irrespective of the motion of the accretion disk at large scales. This choice preserves the direction of rotation of the fluid in the inner accretion flow across all models (see Figure 5 in EHTC V and Wong et al (2021)). We have performed the ray tracing anew, using 200 images across the periods of quiescence identified in EHTC V and decomposing emission into n = 0 and n = 1 sub-images at a resolution of 1/3 µas.…”

Section: Grmhd Resultsmentioning

confidence: 99%

Photon Ring Symmetries in Simulated Linear Polarization Images of Messier 87*

Palumbo,

Wong

2022

Preprint

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The Event Horizon Telescope (EHT) recently released the first linearly polarized images of the accretion flow around the supermassive black hole Messier 87*, hereafter M 87*. The spiraling polarization pattern found in EHT images favored magnetically arrested disks (MADs) as the explanation for the EHT image. With nextgeneration improvements to very long baseline interferometry (VLBI) on the horizon, understanding similar polarized features in the highly lensed structure known as the "photon ring," where photons make multiple halforbits about the black hole before reaching the observer, will be critical to analysis of future images. Recent work has indicated that this image region may be depolarized relative to more direct emission. We expand this observation by decomposing photon half-orbits in the EHT library of simulated images of the M 87* accretion system and find that images of MAD simulations show a relative depolarization of the photon ring attributable to destructive interference of oppositely spiraling electric field vectors; this antisymmetry, which arises purely from strong gravitational lensing, can produce up to ∼50% depolarization in the photon ring region with respect to the direct image. In systems that are not magnetically arrested and with the exception of systems with high spin and ions and electrons of equal temperature, we find that highly lensed indirect sub-images are almost completely depolarized, causing a modest depolarization of the photon ring region in the complete image. We predict that next-generation EHT observations of M 87* polarization should jointly constrain the black hole spin and the underlying emission and magnetic field geometry.

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“…These magnetic flux eruptions could explain the flare events observed in Sgr A* because they are associated with magnetic reconnection, which provides particle heating and acceleration during the flare events and contains enough energy to power flares. Wong et al [118] have investigated the jet-disk boundary layer in different black hole spins and different accretion states, including SANE and MAD. They have shown that in the retrograde case, due to strong shear, the jet-disk boundary is unstable.…”

Section: Grmhd Simulations In the Mad Regimementioning

confidence: 99%

GRMHD Simulations and Modeling for Jet Formation and Acceleration Region in AGNs

Mizuno

2022

Universe

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Relativistic jets are collimated plasma outflows with relativistic speeds. Astrophysical objects involving relativistic jets are a system comprising a compact object such as a black hole, surrounded by rotating accretion flows, with the relativistic jets produced near the central compact object. The most accepted models explaining the origin of relativistic jets involve magnetohydrodynamic (MHD) processes. Over the past few decades, many general relativistic MHD (GRMHD) codes have been developed and applied to model relativistic jet formation in various conditions. This short review provides an overview of the recent progress of GRMHD simulations in generating relativistic jets and their modeling for observations.

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The Jet–disk Boundary Layer in Black Hole Accretion

Cited by 26 publications

References 49 publications

Jets in Magnetically Arrested Hot Accretion Flows: Geometry, Power and Black Hole Spindown

Jets in Magnetically Arrested Hot Accretion Flows: Geometry, Power and Black Hole Spindown

Photon Ring Symmetries in Simulated Linear Polarization Images of Messier 87*

GRMHD Simulations and Modeling for Jet Formation and Acceleration Region in AGNs

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