The Variability of the Black-Hole Image in M87 at the Dynamical Timescale

Positron Effects on Polarized Images and Spectra from Jet and Accretion Flow Models of M87 and Sgr A* (v1) (v2) (v3) (v4)

Event Horizon Telescope observations of the jet launching and collimation in Centaurus A

Constraints on black-hole charges with the 2017 EHT observations of M87*

Broadband Multi-Wavelength Properties of M87 During the 2017 Event Horizon Telescope Campaign

First Event Horizon Telescope Results. VIII. Magnetic Field Structure Near the Event Horizon

First Event Horizon Telescope Results. VII. Polarization of the Ring

Polarimetric Properties of Event Horizon Telescope Targets from ALMA

On the Comparison of AGN with GRMHD Simulations. I: Sgr A* (v1) (v2)

Determining the Composition of Relativistic Jets from Polarization Maps (v1) (v2)

A Quasi-Static Hyper-Resistive Model of UHE Cosmic Ray Acceleration by Magnetically Collimated Jets Created by AGN (v1) (v2)

Multiwavelength Observations of Relativistic Jets from General Relativistic Magnetohydrodynamic Simulations

The Future of Black Hole Astrophysics in the LIGO-VIRGO-LPF Era

Towards Multiwavelength Observations of Relativistic Jets from General Relativistic Magnetohydrodynamic Simulations (Stanford PhD Thesis)

Minute-Timescale >100MeV Gamma Ray Variability During the Giant Outburst of Quasar 3C 279 Observed by FERMI-LAT in June 2015

The Pauli Exclusion Principle at Strong Coupling – Holographic Matter and Momentum Space

TeV gamma rays from distant BL-Lacs and photon-paraphoton kinetic mixing

Grand Unification Scale Primordial Black Holes – Consequences and Constraints

Cover Story (view full-size image) M87 jet magnetic flux tubes are observed here at 15 GHz by the VLBA (courtesy of Kellermann, K.; et al.), possibly indicative of the magnetic Kelvin-Helmholtz instability. This pattern also appears in simulation models (Anantua et al. 2018) when the energy density of relativistic electrons in the radio jet does not decline with magnetic field strength at increasing radii from the black hole. With observation length scales over an order of magnitude greater than simulation scales, more remote processes such as coupling to the rotating interstellar medium may be responsible for the twisting flux tubes observed than in the simulation. Finite VLBA imaging resolution may restrict observers to seeing only the largest structures (the m = ±1 modes), while it may be possible to resolve smaller-scale structure in simulations. With the “Observing” Jet/Accretion Disk/Black Hole (JAB) simulations methodology, we may analyze disk/jet magnetohydrodynamic interactions to be exhibited by the EHT.

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