English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We study the observational signatures of magnetically arrested black holeaccretion with non-rotating inflow onto a rotating black hole; we consider arange of angles between the black hole spin and the initial magnetic fieldorientation. We compare the results of our General RelativisticMagneto-Hydrodynamic simulations to more commonly used rotating initialconditions and to the Event Horizon Telescope (EHT) observations of M87. Wefind that the mm intensity images, polarization images, and synchrotronemission spectra are very similar among the different simulations whenpost-processed with the same electron temperature model; observationaldifferences due to different electron temperature models are significantlylarger than those due to the different realizations of magnetically arrestedaccretion. The orientation of the mm synchrotron polarization is particularlyinsensitive to the initial magnetic field orientation, the electron temperaturemodel, and the rotation of the inflowing plasma. The largest difference amongthe simulations with different initial rotation and magnetic tilt is in thestrength and stability of the jet; spherical inflow leads to kink-unstablejets. We discuss the implications of our results for current and future EHTobservations and for theoretical models of event-horizon-scale black holeaccretion.

Observational Signatures of Black Hole Accretion: Rotating vs. Spherical Flows with Tilted Magnetic Fields