Modeling Polarized Emission from Black Hole Jets: Application to M87 Core Jet

Mościbrodzka, Monika

doi:10.3390/galaxies5030054

Cited by 3 publications

(3 citation statements)

References 46 publications

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“…This will be our only physical assumption and it will lead us to a clear signature. It would be interesting to find an example of a physical mechanism that would produce such a polarization profile at the source-in the interim, we simply note that traditional simulations also appear to predict a whorl-like pattern in certain regimes [22][23][24]27].…”

Section: (C) Symmetric Source Polarizationmentioning

confidence: 96%

“…The optical appearance of the black hole is largely determined by the brightness of the surrounding emission region, and has been the focus of intense investigation [12][13][14][15][16][17]. The EHT will also measure the polarization of incident light, which is expected to carry important information about dynamics in the region surrounding the black hole [18][19][20][21][22][23][24][25][26][27]. The present work concerns this polarimetric image, which has received comparatively less attention.…”

Section: Introductionmentioning

confidence: 99%

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Polarization whorls from M87* at the event horizon telescope

et al. 2020

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The event horizon telescope (EHT) is expected to soon produce polarimetric images of the supermassive black hole at the centre of the neighbouring galaxy M87. There are indications that this black hole is rapidly spinning. General relativity predicts that such a high-spin black hole has an emergent conformal symmetry near its event horizon. In this paper, we use this symmetry to analytically predict the polarized near-horizon emissions to be seen at the EHT and find a distinctive pattern of whorls aligned with the spin.

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Section: (C) Symmetric Source Polarizationmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

Polarization whorls from M87* at the event horizon telescope

et al. 2020

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“…Impelled by the forthcoming EHT observations of Sgr A * and the radio core of M 87, spectra and images of the accretion disc/BH/jet system are currently being performed by post-processing GRMHD simulations using relativistic radiative transfer (for radiative processes such as synchrotron emission, self-absorption, and inverse-Compton processes) and ray-tracing including general relativistic effects ( [101] and references therein; see also Figure 3) after modeling the location-dependent distribution functions of the emitting particles. However, it is important to note that, despite the huge advances experienced by the numerical simulation of the jet formation process, they still suffer from important theoretical uncertainties.…”

Section: General Relativistic Radiative Transfer Simulationsmentioning

confidence: 99%

Numerical Simulations of Jets from Active Galactic Nuclei

Martí

2019

Galaxies

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Numerical simulations have been playing a crucial role in the understanding of jets from active galactic nuclei (AGN) since the advent of the first theoretical models for the inflation of giant double radio galaxies by continuous injection in the late 1970s. In the almost four decades of numerical jet research, the complexity and physical detail of simulations, based mainly on a hydrodynamical/magneto-hydrodynamical description of the jet plasma, have been increasing with the pace of the advance in theoretical models, computational tools and numerical methods. The present review summarizes the status of the numerical simulations of jets from AGNs, from the formation region in the neighborhood of the supermassive central black hole up to the impact point well beyond the galactic scales. Special attention is paid to discuss the achievements of present simulations in interpreting the phenomenology of jets as well as their current limitations and challenges.

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Linear polarization in the nucleus of M87 at 7 mm and 1.3 cm

Kravchenko

Giroletti

Hada

et al. 2020

A&A

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We report on high angular resolution polarimetric observations of the nearby radio galaxy M87 using the Very Long Baseline Array at 24 GHz (λ = 1.3 cm) and 43 GHz (λ = 7 mm) in 2017–2018. New images of the linear polarization substructure in the nuclear region are presented, characterized by a two-component pattern of polarized intensity and smooth rotation of the polarization plane around the 43 GHz core. From a comparison with an analogous dataset from 2007, we find that this global polarization pattern remains stable on a time interval of 11 yr, while showing smaller month-scale variability. We discuss the possible Faraday rotation toward the M87 nucleus at centimeter to millimeter wavelengths. These results can be interpreted in a scenario where the observed polarimetric pattern is associated with the magnetic structure in the confining magnetohydrodynamic wind, which also serves as the source of the observed Faraday rotation.

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Modeling Polarized Emission from Black Hole Jets: Application to M87 Core Jet

Cited by 3 publications

References 46 publications

Polarization whorls from M87* at the event horizon telescope

Polarization whorls from M87* at the event horizon telescope

Numerical Simulations of Jets from Active Galactic Nuclei

Linear polarization in the nucleus of M87 at 7 mm and 1.3 cm

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