Toward a Full MHD Jet Model of Spinning Black Holes. I. Framework and a Split Monopole Example

Huang, Lei; Pan, Zhen; Yu, Cong

doi:10.3847/1538-4357/ab2909

Cited by 10 publications

(11 citation statements)

References 108 publications

(181 reference statements)

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“…Here, 6) is identical with Equation (34) in Pu et al (2015) and Equation ( 23) in Huang et al (2019).…”

Section: Bernoulli Equationmentioning

confidence: 99%

“…To solve the GS equation is computationally demanding (Nitta et al 1991;Fendt 1997;Beskin 2010;Nathanail & Contopoulos 2014;Pan et al 2017;Mahlmann et al 2018). Recently, Huang et al (2019) and Huang et al (2020) succeeded in constructing steady axisymmetric numerical solutions for the monopole and parabolic field line configurations by iteratively solving the wind equation and the GS equa-tion. In Huang et al (2020), they introduced the 'loading zone'.…”

Section: Introductionmentioning

confidence: 99%

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Matter density distribution of general relativistic highly magnetized jets driven by black holes

Ogihara,

Ogawa,

Toma

2021

Preprint

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High-resolution very long baseline interferometry (VLBI) radio observations have resolved the detailed emission structures of active galactic nucleus jets. General relativistic magnetohydrodynamic (GRMHD) simulations have improved the understanding of jet production physics, although theoretical studies still have difficulties in constraining the origin and distribution of jetted matter. We construct a new steady, axisymmetric GRMHD jet model to obtain approximate solutions of black hole (BH) magnetospheres, and examine the matter density distribution of jets. By assuming fixed poloidal magnetic field shapes that mimic force-free analytic solutions and GRMHD simulation results and assuming constant poloidal velocity at the separation surface, which divides the inflow and outflow, we numerically solve the force-balance between the field lines at the separation surface and analytically solve the distributions of matter velocity and density along the field lines. We find that the densities at the separation surface in our parabolic field models roughly follow ∝ r −2 ss in the far zone from the BH, where r ss is the radius of the separation surface. When the BH spin is larger or the velocity at the separation surface is smaller, the density at the separation surface becomes concentrated more near the jet edge. Our semi-analytic model, combined with radiative transfer calculations, may help interpret the high-resolution VLBI observations and understand the origin of jetted matter.

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“…Here, 6) is identical with Equation (34) in Pu et al (2015) and Equation ( 23) in Huang et al (2019).…”

Section: Bernoulli Equationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Matter density distribution of general relativistic highly magnetized jets driven by black holes

Ogihara,

Ogawa,

Toma

2021

Preprint

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“…The choice of Φ, which determines the toroidal magnetic field, is important (e.g., Sulkanen & Lovelace 1990;Camenzind 1987). Physically, it is the rotation which develops a toroidal magnetic field and poloidal electric field in the lab frame (or the inertial frame), which seems to imply that Φ would not be chosen arbitrarily and would be self-consistently determined by the MHD equations, given Ψ and Ω specified (e.g., Beskin & Tchekhovskoy 2005;Contopoulos et al 2013;Huang et al 2019). To solve the rotation term Equation 11, one can see that in the case of…”

Section: φ φ ωmentioning

confidence: 99%

Analytical Solution of Magnetically Dominated Astrophysical Jets and Winds: Jet Launching, Acceleration, and Collimation

Chen,

Zhang

2020

Preprint

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We present an analytical solution of a highly magnetized jet/wind flow. The left-hand of the general force-free jet/wind equation (the "pulsar" equation) is separated into a rotating and a non-rotating term. The two equations with either term can be solved analytically and the two solutions match each other very well. Therefore, we obtain a general approximate solution of a magnetically dominated jet/wind, which covers from the non-relativistic to relativistic regimes, with the drift velocity well matching the cold plasma velocity. The acceleration of a jet includes three stages. 1. The jet flow is located within the Alfvén critical surface (i.e. the light cylinder), has a non-relativistic speed, and is dominated by toroidal motion. 2. The jet is beyond the Alfvén critical surface where the flow is dominated by poloidal motion and becomes relativistic. The total velocity in these two stages follows the same law vΓ = ΩR. 3. The evolution law is replaced by vΓ ≈ 1/ θ √ 2 − ν , where θ is the half opening angle of the jet and 0 ≤ ν ≤ 2 is a free parameter determined by the magnetic field configuration. This is because the earlier efficient acceleration finally breaks the causality connection between different parts in the jet, preventing a global solution. The jet has to carry local charges and currents to support an electromagnetic balance. This approximate solution is consistent with known theoretical results and numerical simulations and it is more convenient to directly compare with observations. This theory may be used to constrain the spin of black holes in astrophysical jets.

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“…Despite recent progress on the magnetohydrodynamics (MHD) of rotating black holes (e.g. Yao et al (2021), Huang et al (2019), Pu & Takahashi (2020)), several properties of their plasma-filled magnetospheres are not completely known. In particular, the energy release at the base of jets associated with Active Galactic Nuclei (AGN) and Gamma Ray Bursts (GRB) may be explained via several mechanisms, depending on the geometry and the physical content of the black hole magnetosphere.…”

Section: Introductionmentioning

confidence: 99%

Double flows anchored in a Kerr black hole horizon – I. Meridionally self-similar MHD models with loading terms

Chantry

Cayatte

Sauty

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Recent observations of supermassive black holes have brought us new information on their magnetospheres. In this study we attempt a theoretical modelling of the coupling of black holes with their jets and discs, via three innovations. First, we propose a semi-analytical MHD description of a steady relativistic inflow-outflow structure characteristic to the extraction of the hole rotational energy. The mass-loading is ensured in a thin layer, the stagnation surface, by a two-photon pair production originating to a gamma-ray emission from the surrounding disc. The double flow is described near the polar axis by an axisymmetric meridionally self-similar MHD model. Second, the inflow and outflow solutions are crossing the MHD critical points and are matched at the stagnation surface. Knowledge of the MHD field on the horizon give us the angular momentum and energy extracted from the black hole. Finally, we illustrate the model with three specific examples of double-flow solutions by varying the energetic interaction between the MHD field and the rotating black hole. When the isorotation frequency is half of the black hole one, the extracted Poynting flux is comparable to the one obtained using the force-free assumption. In two of the presented solutions, the Penrose process dominates at large colatitudes, while the third is Poynting flux dominated at mid colatitudes. Mass injection rate estimations, from disk luminosity and inner radius, give an upper limit just above the values obtained for two solutions. This model is pertinent to describe the flows near the polar axis where pair production is more efficient.

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Toward a Full MHD Jet Model of Spinning Black Holes. I. Framework and a Split Monopole Example

Cited by 10 publications

References 108 publications

Matter density distribution of general relativistic highly magnetized jets driven by black holes

Matter density distribution of general relativistic highly magnetized jets driven by black holes

Analytical Solution of Magnetically Dominated Astrophysical Jets and Winds: Jet Launching, Acceleration, and Collimation

Double flows anchored in a Kerr black hole horizon – I. Meridionally self-similar MHD models with loading terms

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