The first event-horizon-scale image of the M87 black hole shows a 42 microarcsecond diameter ring with a central brightness depression, consistent with the shadow of a Kerr black hole.
Two-temperature, Magnetically Arrested Disc simulations of the jet from the supermassive black hole in M87
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abstract
We present two-temperature, radiative general relativistic magnetohydrodynamic simulations of Magnetically Arrested Discs (MAD) that launch powerful relativistic jets. The mass accretion rates of our simulations are scaled to match the luminosity of the accretion flow around the supermassive black hole in M87. We consider two sub-grid prescriptions for electron heating: one based on a Landau-damped turbulent cascade, and the other based on heating from trans-relativistic magnetic reconnection. The simulations produce jets with power on the order of the observed value for M87. Both simulations produce spectra that are consistent with observations of M87 in the radio, millimetre, and submillimetre. Furthermore, the predicted image core-shifts in both models at frequencies between 15 GHz and 86 GHz are consistent with observations. At 43 and 86 GHz, both simulations produce wide opening angle jets consistent with VLBI images. Both models produce 230~GHz images with distinct black hole shadows that are resolvable by the Event Horizon Telescope (EHT), although at a viewing angle of 17 degrees, the 230 GHz images are too large to match EHT observations from 2009 and 2012. The 230 GHz images from the simulations are dynamic on time-scales of months to years, suggesting that repeated EHT observations may be able to detect the motion of rotating magnetic fields at the event horizon.
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EHT data shows M87's asymmetric ring is consistent with the shadow of a spinning Kerr black hole, with jet power requiring spin-energy extraction via Blandford-Znajek-like processes.
Corotating point sources on accretion disks near black holes distort the relative magnification factor distribution, modulating caustics and encoding accretion flow kinematics via time-delayed images.
Kerr-BR black hole images with magnetically coupled synchrotron emissivity show spin- and B-dependent shifts in the inner disk edge, altered lensing rings, and Doppler asymmetries, with retrograde cases displaying wider central depletion.
Polarization signatures from GRMHD simulations of black hole accretion can help probe disk, corona, and jet properties when combined with X-ray polarimetry observations.
citing papers explorer
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First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole
The first event-horizon-scale image of the M87 black hole shows a 42 microarcsecond diameter ring with a central brightness depression, consistent with the shadow of a Kerr black hole.
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First M87 Event Horizon Telescope Results. V. Physical Origin of the Asymmetric Ring
EHT data shows M87's asymmetric ring is consistent with the shadow of a spinning Kerr black hole, with jet power requiring spin-energy extraction via Blandford-Znajek-like processes.
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Relative Magnification Factor of Point Sources on Accretion Disks
Corotating point sources on accretion disks near black holes distort the relative magnification factor distribution, modulating caustics and encoding accretion flow kinematics via time-delayed images.
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Optical Appearance of the Kerr-Bertotti-Robinson Black Hole with a Magnetically Driven Synchrotron Emissivity Model
Kerr-BR black hole images with magnetically coupled synchrotron emissivity show spin- and B-dependent shifts in the inner disk edge, altered lensing rings, and Doppler asymmetries, with retrograde cases displaying wider central depletion.
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Polarization Signatures from GRMHD Simulations of Black Hole Accretion
Polarization signatures from GRMHD simulations of black hole accretion can help probe disk, corona, and jet properties when combined with X-ray polarimetry observations.