Jet launching radius in low-power radio-loud AGNs in advection-dominated accretion flows

Le, Truong; Newman, William I.; Edge, Brinkley

doi:10.1093/mnras/sty644

Cited by 6 publications

(7 citation statements)

References 67 publications

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“…LB04; LB05). The value obtained for the shock/jet radius in Model C is r * = 14.78 R g , which is comparable to the jet-launching radius deduced in the case of M87 by Le et al (2018).…”

Section: Particle Distribution In the M87 Jetsupporting

confidence: 79%

“…This has stimulated renewed interest in the possibility of shock-driven outflows. In particular, we note that Le et al (2016), Le et al (2018), and Chattopadhyay & Kumar (2016) confirmed the existence of stable disc/shock configurations with associated shock-driven outflows in ADAF discs.…”

Section: Standing Shocks and Outflows In Adaf Discssupporting

confidence: 64%

“…However, recent studies have shown that this mechanism tends to channel energy into the equatorial plane of the disc, rather than along the rotation axis of the disc, calling into question of the effectiveness of these mechanisms for powering relativistic jets (e.g. Menon & Dermer 2005; Le et al 2018). This has stimulated renewed interest in the possibility of shock-driven outflows.…”

Section: Standing Shocks and Outflows In Adaf Discsmentioning

confidence: 99%

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A two-fluid model for black-hole accretion flows: Particle acceleration, outflows, and TeV emission

Lee

Becker

2019

Monthly Notices of the Royal Astronomical Society

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The multi-wavelength spectrum observed from M87 extends from radio wavelengths up to TeV γ-ray energies. The radio through GeV components have been interpreted successfully using SSC models based on misaligned blazar jets, but the origin of the intense TeV emission detected during flares in 2004, 2005, and 2010 remains puzzling. It has been previously suggested that the TeV flares are produced when a relativistic proton jet originating in the core of M87 collides with a molecular cloud (or stellar atmosphere) located less than one parsec from the central black hole. We explore this scenario in detail here using a self-consistent model for the acceleration of relativistic protons in a shocked, two-fluid ADAF accretion disc. The relativistic protons accelerated in the disc escape to power the observed jet outflows. The distribution function for the jet protons is used to compute the TeV emission produced when the jet collides with a cloud or stellar atmosphere. The simulated broadband radiation spectrum includes radio, X-ray and GeV components generated via synchrotron, as well as TeV emission generated via the production and decay of muons, positrons and electrons. The self-consistency of the model is verified by computing the relativistic particle pressure using the distribution function, and comparing it with the relativistic particle pressure obtained from the hydrodynamical model. We demonstrate that the model is able to reproduce the multi-wavelength spectrum from M87 observed by VERITAS and HESS during the high-energy flares in 2004, 2005, and 2010.

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“…LB04; LB05). The value obtained for the shock/jet radius in Model C is r * = 14.78 R g , which is comparable to the jet-launching radius deduced in the case of M87 by Le et al (2018).…”

Section: Particle Distribution In the M87 Jetsupporting

confidence: 79%

Section: Standing Shocks and Outflows In Adaf Discssupporting

confidence: 64%

Section: Standing Shocks and Outflows In Adaf Discsmentioning

confidence: 99%

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A two-fluid model for black-hole accretion flows: Particle acceleration, outflows, and TeV emission

Lee

Becker

2019

Monthly Notices of the Royal Astronomical Society

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“…Patterson & Raymond 1985;Mukai 2017), accretion shocks (e.g. Fukumura & Kazanas 2007b;Le et al 2016Le et al , 2018 or propagation of nuclear burning on accreting neutron stars (e.g. Spitkovsky et al 2002).…”

Section: Introductionmentioning

confidence: 99%

Iron Line Tomography of General Relativistic Hydrodynamic Accretion around Kerr Black Holes

Porter

Fukumura

2020

ApJ

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We consider a temporal response of relativistically broadened line spectrum of iron from black hole accretion irradiated by an X-ray echo under strong gravity. The physical condition of accreting gas is numerically calculated in the context of general relativistic hydrodynamics under steady-state, axisymmetry in Kerr geometry. With the onset of a point-like X-ray flare of a short finite duration just above the accretion surface, the gas is assumed to be ionized to produce a neutral iron fluorescent line. Using a fully relativistic ray-tracing approach, the response of line photons due to the X-ray illumination is traced as a function of time and energy for different source configurations around Schwarzschild and Kerr black holes. Our calculations show that the X-ray echo on the accretion surface clearly imprints a characteristic time-variability in the line spectral features depending on those parameters. Simulated line profiles, aimed for the future microcalorimeter missions of large collecting area such as Athena/X-IFU for typical radio-quiet Seyfert galaxies, are presented to demonstrate that state-of-the-art new observations could differentiate various source parameters by such an X-ray tomographic line reverberation.

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“…These objects are characterized by trans-or highly relativistic jets, namely having Lorentz factor Γ ≫ 1. Such jets are produced by collapse of a massive star, merger of two compact objects (in the case of GRBs) [11][12][13][14], or through an accretion disc surrounding a black hole [15][16][17][18][19][20][21][22][23][24]. Although the geometric shape of these jets is uncertain, numerical modeling shows some typical jet profiles where the jet's Lorentz factor is a function of its polar angle, [i.e., Γ = Γ(θ)] which may be universal [25][26][27].…”

mentioning

confidence: 99%

Photons' scattering in a relativistic plasma with velocity shear: generation of high energy power-law spectra

Vyas¹,

Pe’er²

2022

Preprint

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A high energy power law is a common feature in the spectra of many astrophysical objects. We show that the photons in a relativistic plasma with a variable Lorentz factor go through repeated scattering with electrons to gain energy. The escaped population of photons naturally produces a power-law-shaped spectrum making it an anisotropic analogue to the conventional Fermi acceleration mechanism of charged particles. Thus, this mechanism provides a natural alternative to current explanations of high energy power-law spectra via synchrotron or thermal Comptonization. The model is applicable to any relativistic plasma beam with an arbitrary Lorentz factor profile. We implement the theory to GRB prompt phase and show that the obtained range of the photon indices is compatible with the observed values. Therefore, the observed high energy spectral indices provide a unique indicator of the jet structure.

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Jet launching radius in low-power radio-loud AGNs in advection-dominated accretion flows

Cited by 6 publications

References 67 publications

A two-fluid model for black-hole accretion flows: Particle acceleration, outflows, and TeV emission

A two-fluid model for black-hole accretion flows: Particle acceleration, outflows, and TeV emission

Iron Line Tomography of General Relativistic Hydrodynamic Accretion around Kerr Black Holes

Photons' scattering in a relativistic plasma with velocity shear: generation of high energy power-law spectra

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