Numerical Modeling of Multi-Wavelength Spectra of M87 Core Emission

Hilburn, Guy; Liang, Edison

doi:10.1088/0004-637x/746/1/87

Cited by 10 publications

(8 citation statements)

References 53 publications

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“…The resulting best fiṫ M will vary depending upon the underlying electron distribution functions in the accretion disk and jet. They typically vary (Mościbrodzka et al 2011, Hilburn & Liang 2012. In our fiducial model RH100, we findṀ = 9 × 10 −3 M yr −1 .…”

Section: Mass-accretion Ratementioning

confidence: 50%

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General relativistic magnetohydrodynamical simulations of the jet in M 87

Mościbrodzka

Falcke

Shiokawa

2016

A&A

307

314

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Context. The connection between black hole, accretion disk, and radio jet can be constrained best by fitting models to observations of nearby low-luminosity galactic nuclei, in particular the well-studied sources Sgr A* and M 87. There has been considerable progress in modeling the central engine of active galactic nuclei by an accreting supermassive black hole coupled to a relativistic plasma jet. However, can a single model be applied to a range of black hole masses and accretion rates? Aims. Here we want to compare the latest three-dimensional numerical model, originally developed for Sgr A* in the center of the Milky Way, to radio observations of the much more powerful and more massive black hole in M 87. Methods. We postprocess three-dimensional GRMHD models of a jet-producing radiatively inefficient accretion flow around a spinning black hole using relativistic radiative transfer and ray-tracing to produce model spectra and images. As a key new ingredient in these models, we allow the proton-electron coupling in these simulations depend on the magnetic properties of the plasma. Results. We find that the radio emission in M 87 is described well by a combination of a two-temperature accretion flow and a hot single-temperature jet. Most of the radio emission in our simulations comes from the jet sheath. The model fits the basic observed characteristics of the M 87 radio core: it is "edge-brightened", starts subluminally, has a flat spectrum, and increases in size with wavelength. The best fit model has a mass-accretion rate ofṀ ∼ 9 × 10 −3 M yr −1 and a total jet power of P j ∼ 10 43 erg s −1 . Emission at λ = 1.3 mm is produced by the counter-jet close to the event horizon. Its characteristic crescent shape surrounding the black hole shadow could be resolved by future millimeter-wave VLBI experiments. Conclusions. The model was successfully derived from one for the supermassive black hole in the center of the Milky Way by appropriately scaling mass and accretion rate. This suggests the possibility that this model could also apply to a wider range of low-luminosity black holes.

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Section: Mass-accretion Ratementioning

confidence: 50%

“…General relativistic radiative transfer (GRRT) models can predict the general relativistic magnetohydrodynamical (GRMHD) simulation spectrum and appearance. This allows us to compare dynamical models directly to VLBI observations (e.g., Dexter et al 2012;Hilburn & Liang 2012;Mościbrodzka et al 2014). …”

Section: Introductionmentioning

confidence: 99%

General relativistic magnetohydrodynamical simulations of the jet in M 87

Mościbrodzka

Falcke

Shiokawa

2016

A&A

307

314

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“…1,58,62 If true, this would most likely argue against an ADAF (bremsstrahlung) origin of the Chandra X-ray variations. 59…”

Section: X-ray Resultsmentioning

confidence: 99%

Probing the Central Black Hole in M87 With Gamma-Rays

Rieger

Aharonian

2012

Mod. Phys. Lett. A

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Recent high-sensitivity observation of the nearby radio galaxy M87 has provided important insights into the central engine that drives the large-scale outflows seen in radio, optical and X-rays. This review summarizes the observational status achieved in the high energy (HE < 100 GeV) and very high energy (VHE > 100 GeV) gamma-ray domains, and discusses the theoretical progress in understanding the physical origin of this emission and its relation to the activity of the central black hole.

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“…Then, Li et al (2009) extended the previous model based on self-similar ADAF solutions in Newtonian approximation and considered GR effects for a HD radiatively inefficient accretion flow (RIAF), which gave a > 0.8. Numerically modelling spectral fits to the M87 core data from radio to hard X-ray under the condition that all the emission goes from the immediate surroundings of the central black hole, Hilburn & Liang (2012) offered the same constraint from the best-fitting parameters. At the same time, Doeleman et al (2012) carried out 1.3-mm VLBI observations of the M87 core and found a full width at half-maximum size of (5.5 ± 0.4)R Sch .…”

Section: Discussionmentioning

confidence: 99%

Black hole spin from wobbling and rotation of the M87 jet and a sign of a magnetically arrested disc

Sob'yanin

2018

Preprint

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New long-term Very Long Baseline Array observations of the well-known jet in the M87 radio galaxy at 43 GHz show that the jet experiences a sideways shift with an approximately 8-10 yr quasi-periodicity. Such jet wobbling can be indicative of a relativistic Lense-Thirring precession resulting from a tilted accretion disc. The wobbling period together with up-to-date kinematic data on jet rotation opens up the possibility for estimating angular momentum of the central supermassive black hole. In the case of a test-particle precession, the specific angular momentum is J/M c = (2.7 ± 1.5) × 10 14 cm, implying moderate dimensionless spin parameters a = 0.5 ± 0.3 and 0.31 ± 0.17 for controversial gas-dynamic and stellar-dynamic black hole masses. However, in the case of a solid-body-like precession, the spin parameter is much smaller for both masses, 0.15 ± 0.05. Rejecting this value on the basis of other independent spin estimations requires the existence of a magnetically arrested disc in M87.

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Numerical Modeling of Multi-Wavelength Spectra of M87 Core Emission

Cited by 10 publications

References 53 publications

General relativistic magnetohydrodynamical simulations of the jet in M 87

General relativistic magnetohydrodynamical simulations of the jet in M 87

Probing the Central Black Hole in M87 With Gamma-Rays

Black hole spin from wobbling and rotation of the M87 jet and a sign of a magnetically arrested disc

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