Accretion of the relativistic Vlasov gas in the equatorial plane of the Kerr black hole

Cieślik, Adam; Mach, Patryk; Odrzywołek, A.

doi:10.1103/physrevd.106.104056

Cited by 9 publications

(5 citation statements)

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“…The case of unbound trajectories has been analyzed in detail in [10] and applied to accretion problems [10,21,[23][24][25][26], see also [22] for the analogous problem on the Reissner-Nordström background and [27] for a thin accretion disk confined to the equatorial plane of a Kerr black hole.…”

Section: Collisionless Gas Configurations Trapped In a Schwarzschild ...mentioning

confidence: 99%

“…In this sense, the work in [19] suggests that (for small enough amplitude) our configurations can likely be generalized to include their self-gravity. We also mention related recent work on the accretion of a Vlasov gas by a central black hole [10,[21][22][23][24][25][26][27] in which unbounded (instead of bounded) timelike geodesics are relevant.…”

Section: Introductionmentioning

confidence: 99%

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Axisymmetric, stationary collisionless gas configurations surrounding Schwarzschild black holes

Fajardo

Sarbach²

2023

Class. Quantum Grav.

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The properties of a stationary gas cloud surrounding a black hole are discussed, assuming that the gas consists of collisionless, identical massive particles that follow spatially bound geodesic orbits in the Schwarzschild spacetime. Several models for the one-particle distribution function are considered, and the essential formulae that describe the relevant macroscopic observables, like the current density four-vector and the stress-energy-momentum tensor are derived. This is achieved by rewriting these observables as integrals over the constants of motion and by a careful analysis of the range of integration. In particular, we provide conﬁgurations with ﬁnite total mass and angular momentum. Differences between these conﬁgurations and their nonrelativistic counter-parts in a Newtonian potential are analyzed. Finally, our conﬁgurations are compared to their hydrodynamic analogues, the “polish doughnuts”.

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Section: Collisionless Gas Configurations Trapped In a Schwarzschild ...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Axisymmetric, stationary collisionless gas configurations surrounding Schwarzschild black holes

Fajardo

Sarbach²

2023

Class. Quantum Grav.

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“…( 124) and (125) in Ref. [25] for Maxwell-Jüttner particle temperatures approaching infinity and Schwarzschild BHs [again set α ≡ a/M = 0 and note ρ s,∞ ≡ Σ ∞ in Eq. (124) and ǫ s,∞ = Σ ∞ E ∞ in Eq.…”

Section: Massless and Extremely Relativistic Particlesmentioning

confidence: 99%

“…Infinite, unbound collisionless clusters around Schwarzschild BHs have been previously investigated with a different approach in Refs [23,24], who adopted a Maxwell-Jünter phase-space distribution function as an application. A treatment involving thin (equatorial plane) disks around Kerr black holes was recently provided by Ref [25], again with a Maxwell-Jünter distribution function and a different approach from the one adopted here. We compare the accretion rates found by these studies with the ones calculated here.…”

Section: Introductionmentioning

confidence: 99%

Spikes and accretion of unbound, collisionless matter around black holes

Shapiro

2023

Phys. Rev. D

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We consider the steady-state density and velocity dispersion profiles of collisionless matter around a Schwarzschild black hole (BH) and its associated rate of accretion onto the BH. We treat matter, which could be stars or dark matter particles, whose orbits are unbound to the BH, but still governed by its gravitational field. We consider two opposite spatial geometries for the matter distributions: an infinite, 3D cluster and a 2D razor-thin disk, both with zero net angular momentum. We demonstrate that the results depend critically on the adopted geometry, even in the absence of angular momentum. We adopt a simple monoenergetic, isotropic, phase-space distribution function for the matter as a convenient example to illustrate this dependence. The effect of breaking strict isotropy by incorporating an unreplenished loss cone due to BH capture of low-angular momentum matter is also considered. Calculations are all analytic and performed in full general relativity, though key results are also evaluated in the Newtonian limit. We consider one application to show that the rate of BH accretion from an ambient cluster can be significantly less than that from a thin disk to which it may collapse, although both rates are considerably smaller than Bondi accretion for a (collisional) fluid with a similar asymptotic particle density and velocity dispersion (i.e., sound speed).

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“…In [39,40], exact solutions were derived for shells accreted onto a Schwarzschild black hole. Recently, exact solutions were presented for the accretion of collisionless Vlasov gas onto a moving Schwarzschild black hole [41,42] or a Schwarzschild-like black hole [43] or a Kerr black hole [44], based on the Hamiltonian formalism developed in [45]. This method enables the analysis of more complex flows on a fixed background.…”

Section: Introductionmentioning

confidence: 99%

Accretion of matter by a charged dilaton black hole

Jia,

He,

Wang

et al. 2024

Eur. Phys. J. C

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Considering accretion onto a charged dilaton black hole, the fundamental equations governing accretion, general analytic expressions for critical points, critical velocity, critical speed of sound, and ultimately the mass accretion rate are obtained. A new constraint on the dilation parameter coming from string theory is found and the case for polytropic gas is delved into a detailed discussion. It is found that the dialtion and the adiabatic index of accreted material have deep effects on the accretion process.

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Accretion of the relativistic Vlasov gas in the equatorial plane of the Kerr black hole

Cited by 9 publications

References 50 publications

Axisymmetric, stationary collisionless gas configurations surrounding Schwarzschild black holes

Axisymmetric, stationary collisionless gas configurations surrounding Schwarzschild black holes

Spikes and accretion of unbound, collisionless matter around black holes

Accretion of matter by a charged dilaton black hole

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